Lista de estrelas e anãs marrons mais próximas: diferenças entre revisões

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[[File:RedDwarfNASA-hue-shifted.jpg|thumb|right|300px|Representação artística de uma estrela [[anã vermelha]], o tipo mais comum de estrela na vizinhança do Sol, e no universo. Apesar do nome, a temperatura superficial desse tipo de estrela daria a ela um tom alaranjado quando vista de perto.]]
{{Sem-fontes|data=junho de 2011| ciência=s}}


Esta '''lista de estrelas próximas''' contém todas as [[estrela]]s e [[anã marrom|anãs marrons]] conhecidas a uma distância de até 5 [[parsec]]s (16,3 [[ano-luz|anos-luz]]) do [[Sistema Solar]], ordenadas por distância crescente. Além do Sistema Solar, há outros 53 [[sistema estelar|sistemas estelares]] conhecidos atualmente a até essa distância. Esses sistemas contêm um total de 60 estrelas que fundem hidrogênio e 12 anãs marrons. Apesar de estarem relativamente próximos da Terra, apenas nove desses objetos têm uma [[magnitude aparente]] menor que 6,5, o que significa que somente 13% deles podem ser vistos a [[olho nu]].<ref>{{cite journal
Esta é uma '''lista de estrelas próximas''' da [[Terra]].
| last=Weaver | first=Harold F.
| title=The Visibility of Stars Without Optical Aid
| journal=Publications of the Astronomical Society of the Pacific
| year=1947 | volume=59 | issue=350 | pages=232–243
| bibcode=1947PASP...59..232W
| doi=10.1086/125956 }}</ref> Além do Sol, há apenas três [[anexo:lista das estrelas mais brilhantes|estrela de primeira magnitude]]: [[Alpha Centauri]], [[Sirius]], e [[Procyon]]. Todos esses objetos estão localizados na [[Bolha Local]], uma região no [[Braço de Órion]] da [[Via Láctea]].


==Lista==
O [[Sol]] é a [[estrela]] mais próxima da Terra, estando a aproximadamente 8 minutos-luz de distância.
Estrelas visíveis a olho nu têm a magnitude aparente destacada em azul claro. Os [[classificação estelar|tipos espectrais]] das estrelas e anãs marrons são mostrados com sua cor correspondente (essas cores são derivadas do nome convencional das classes espectrais e não representam a cor observada da estrela). Muitas anãs marrons não estão listadas por [[espectro visível|magnitude visível]] mas sim por magnitude na [[banda J]]. Algumas [[paralaxe]]s e distância são medições preliminares.<ref name="RECONS">{{cite journal | last = [[Research Consortium on Nearby Stars]] | first = [[Georgia State University|GSU]] | date = 2007-09-17 | title = The One Hundred Nearest Star Systems | journal = [http://www.chara.gsu.edu/RECONS/ RECONS] | url = http://www.chara.gsu.edu/RECONS/TOP100.posted.htm | accessdate = 06/11/2007}}</ref>
A tabela que segue mostra as estrelas mais próximas da Terra, exceto o Sol.
{| style="font-size: 100%; text-align: center;" class="sortable wikitable" border = "1"

{| class="wikitable"
! rowspan="2" |#
! rowspan="2" |#
! colspan="2" |<small>Designação</small>
! class="unsortable" colspan="3" |<small>Designação</small>
! rowspan="2" |<small>[[Classificação estelar|Tipo espectral]]
! rowspan="2" |<small>[[Classificação estelar]]</small>
! rowspan="2" |<small>[[Magnitude aparente|''m'']]</small>
! rowspan="2" |<small>[[Magnitude aparente]] ({{nowrap|m<sub>[[Sistema fotométrico UBV|V]]</sub> ou m<sub>[[banda J|J]]</sub>}})</small>
! rowspan="2" |<small>[[Magnitude absoluta|''M'']]</small>
! rowspan="2" |<small>[[Magnitude absoluta]] ({{nowrap|M<sub>[[Sistema fotométrico UBV|V]]</sub> ou M<sub>[[banda J|J]]</sub>}})</small>
! class="unsortable" style="background: #FFC" colspan="2" |<small>[[Época (astronomia)|Época]] J2000.0</small>
! rowspan="2" |<small>[[Temperatura efetiva|''T<sub>eff</sub>'']]</br>[[kelvin|(K)]]</small>
! rowspan="2" |<small>[[Ascensão reta|AR]]</small>
! rowspan="2" |<small>[[Paralaxe]]<ref name="RECONS"/><br>[[segundo de arco|mas]][[margem de erro|(±err)]]</small>
! rowspan="2" |<small>[[Declinação|Dec]]</small>
! rowspan="2" |<small>Distância<ref name=distfn>Calculada a partir do paralaxe.</ref><br>[[ano-luz|anos-luz]] [[margem de erro|(±err)]]</small>
! rowspan="2" |<small>[[Paralaxe]]</br>[[Segundo de arco|(arcsec)]]</small>
! rowspan="2" |<small>Notas adicionais</small>
|-class="unsortable"
! rowspan="2" |<small>[[Distância]] da [[Terra]]</br>[[Ano-luz|(al)]]</small>
!<small>[[Sistema estelar|Sistema]]</small>
!<small>[[Estrela]]</small>
!<small>Estrela #</small>
!<small>[[Ascensão reta]]<ref name=RECONS/></small>
!<small>[[Declinação]]<ref name=RECONS/></small>
|-
|-
|
!<small>Sistema</small>
| [[Sistema Solar]]
!<small>Estrela</small>
| [[Sol]]
|
| style="background: {{estrela-cor|G}};" | [[anã amarela|G2V]]<ref name=RECONS/>
| style="background: lightblue;" | −26,74<ref name=RECONS/>
| 4,85<ref name=RECONS/>
| colspan="2" | —
| —
| 0
| tem oito planetas
|-
|-
| rowspan="3" | 1
| rowspan="3" | 1
| rowspan="3" | [[Alfa do Centauro|Alfa Centauri]]
| rowspan="3" | [[Alpha Centauri]]<br>(Rigil&nbsp;Kentaurus)
| style="background-color: #CCC;" | [[Proxima Centauri|Próxima Centauri]] (V645 Centauri)
| [[Proxima Centauri|Proxima&nbsp;Centauri]] (V645&nbsp;Centauri)
| 1
| style="background-color: #F99;" | [[Anã vermelha|M5.5Ve]]
| style="background: {{estrela-cor|M}};" | [[Anã vermelha|M5.5Ve]]
| 11.01
| 11,09<ref name=RECONS />
| 15.53
| 15,53<ref name=RECONS />
| 2670
| {{RA|14|29|43}}
| {{RA|14|29|43,0}}
| {{DEC|−62|40|46}}
| {{DEC|−62|40|46}}
| align=left | 768,87(029)<ref name="Y">[[General Catalogue of Trigonometric Parallaxes]].</ref><ref name="H">[[Catálogo Hipparcos]].</ref>
| 0.768 9(0 3)″
| 4.2420(16)
| 4,2421(16)
| <ref name="B">Burgasser et al. 2000</ref>
|-
|-
| [[Alfa Centauri|Alfa Centauri A]] (Rigil Kentaurus; Toliman)
| α&nbsp;Centauri&nbsp;A (HD&nbsp;128620)
| 2
| style="background-color: #FF9;" | [[Anã amarela|G2V]]
| style="background: {{estrela-cor|G}};" | [[anã amarela|G2V]]<ref name=RECONS />
| −0.01
| style="background: lightblue;" | 0,01<ref name=RECONS />
| 4.38
| 4,38<ref name=RECONS />
| 5800
| {{RA|14|39|37}}
| {{RA|14|39|36,5}}
| {{DEC|−60|50|2}}
| {{DEC|−60|50|02}}
| rowspan="2" align=left | 747,23(117)<ref name="Y"/><ref name="S">[http://adsabs.harvard.edu/abs/1999A%26A...341..121S Visual binary orbits and masses post Hipparcos], Staffan Söderhjelm, ''Astronomy and Astrophysics'' '''341''' (janeiro de 1999), pp. 121&ndash;140.</ref>
| rowspan="2" | 0.747 2(1 2)″
| rowspan="2" | 4.3649(69)
| rowspan="2" | 4,3650(68)
| rowspan="2" |
|-
|-
| [[Alfa Centauri|Alfa Centauri B]] (HD 128621)
| α&nbsp;Centauri&nbsp;B (HD&nbsp;128621)
| 2
| style="background-color: #FC9;" | [[Anã laranja|K0V]]
| style="background: {{estrela-cor|K}};" | [[anã laranja|K1V]]<ref name=RECONS />
| 1.35
| style="background: lightblue;" | 1,34<ref name=RECONS />
| 5.71
| 5,71<ref name=RECONS />
| 5300
| {{RA|14|39|35}}
| {{RA|14|39|35,1}}
| {{DEC|−60|50|14}}
| {{DEC|−60|50|14}}
|-
|-
| 2
| style="background-color: #CCC;" | 2
| colspan="2" style="background-color: #CCC;" | [[Estrela de Barnard]] (BD+04°3561a)
| colspan="2" | [[Estrela de Barnard]] (BD+04°3561a)
| 4
| style="background-color: #F99;" | M4.0Ve
| style="background: {{estrela-cor|M}};" | M4.0Ve
| 9.53
| 9,53<ref name=RECONS />
| 13.22
| 13,22<ref name=RECONS />
| 3134
| {{RA|17|57|48}}
| {{RA|17|57|48,5}}
| {{DEC|+04|41|36}}
| {{DEC|+04|41|36}}
| align=left | 546,98(1&nbsp;00)<ref name="Y"/><ref name="H"/>
| 0.547 0(1 0)″
| 5.9629(110)
| 5,9630(109)
|
|-
|-
| 3
| style="background-color: #CCC;" | 3
| colspan="2" style="background-color: #CCC;" | [[Wolf 359]] (CN Leonis)
| colspan="2" | [[Wolf 359|Wolf&nbsp;359]] (CN&nbsp;Leonis)
| 5
| style="background-color: #F99;" | M6.0V
| style="background: {{estrela-cor|M}};" | M6.0V<ref name=RECONS />
| 13.44
| 13,44<ref name=RECONS />
| 16.55
| 16,55<ref name=RECONS />
| 3500
| {{RA|10|56|28}}
| {{RA|10|56|29,2}}
| {{DEC|+07|00|42}}
| {{DEC|+07|00|53}}
|align=left | 419,10(210)<ref name="Y" />
| 0.419 1(2 1)″
| 7.7823(390)
| 7,7825(390)
|
|-
|-
| 4
| style="background-color: #CCC;" | 4
| colspan="2" style="background-color: #CCC;" | [[Lalande 21185]] (BD+36°2147)
| colspan="2" | [[Lalande 21185|Lalande&nbsp;21185]] (BD+36°2147)
| 6
| style="background-color: #F99;" | M2.0V
| style="background: {{estrela-cor|M}};" | M2.0V<ref name=RECONS />
| 7.47
| 7,47<ref name=RECONS />
| 10.44
| 10,44<ref name=RECONS />
| 3400
| {{RA|11|00|37}}
| {{RA|11|03|20,2}}
| {{DEC|+36|18|20}}
| {{DEC|+35|58|12}}
| align=left | 393,42(070)<ref name="Y"/><ref name="H"/>
| 0.393 4(0 7)″
| 8.2903(148)
| 8,2905(148)
|
|-
|-
| rowspan="2" | 5
| rowspan="2" | 5
| rowspan="2" | [[Sirius]]
| rowspan="2" | [[Sirius]]<br>(α&nbsp;Canis&nbsp;Majoris)
| Sirius A (α Canis Majoris)
| Sirius A
| 7
| bgcolor="ffffff" | [[Estrela branca da sequência principal|A1V]]
| style="background: {{estrela-cor|A}}" | [[estrela branca da sequência principal|A1V]]<ref name=RECONS />
| −1.47
| style="background: lightblue;" | −1,46<ref name=RECONS />
| 1.48
| 1,42<ref name=RECONS />
| 9900
| rowspan="2" | {{RA|06|45|09}}
| rowspan="2" | {{RA|06|45|08,9}}
| rowspan="2" | {{DEC|−16|42|58}}
| rowspan="2" | {{DEC|−16|42|58}}
| rowspan="2" | 0.380 0(1 3)″
| rowspan="2" align=left | 380,02(128)<ref name="Y"/><ref name="H"/>
| rowspan="2" | 8.5826(290)
| rowspan="2" | 8,5828(289)
| rowspan="2" |
|-
|-
| Sirius&nbsp;B
| style="background-color: #CCC;" | Sirius B
| 7
| bgcolor="F0F0F0" | [[Anã branca|DA2]]
| style="background: F0F0F0" | [[Anã branca|DA2]]<ref name=RECONS />
| 8.44
| 8,44<ref name=RECONS />
| 11.34
| 11,34<ref name=RECONS />
| 25200
|-
|-
| rowspan="2" style="background-color: #CCC;" | 6
| rowspan="2" | 6
| rowspan="2" style="background-color: #CCC;" | [[Luyten 726-8]]
| rowspan="2" | [[Luyten 726-8|Luyten&nbsp;726-8]]
| Luyten&nbsp;726-8&nbsp;A (BL&nbsp;Ceti)
| style="background-color: #CCC;" | UV Ceti (L 726-8 B)
| 9
| style="background-color: #F99;" | M5.5Ve
| style="background: {{estrela-cor|M}};" | M5.5Ve
| 12.54
| 12,54<ref name=RECONS />
| 15.40
| 15,40<ref name=RECONS />
| ~2700
| rowspan="2" | {{RA|01|39|01}}
| rowspan="2" | {{RA|01|39|01,3}}
| rowspan="2" | {{DEC|−17|57|00}}
| rowspan="2" | {{DEC|−17|57|01}}
| rowspan="2" | 0.373 7(2 7)″
| rowspan="2" align=left | 373,70(270)<ref name="Y"/>
| rowspan="2" | 8.7278(631)
| rowspan="2" | 8,7280(631)
| rowspan="2" |
|-
|-
| Luyten&nbsp;726-8&nbsp;B (UV&nbsp;Ceti)
| style="background-color: #CCC;" | BL Ceti (L 726-8 A)
| 10
| style="background-color: #F99;" | M6.0Ve
| style="background: {{estrela-cor|M}};" | M6.0Ve
| 12.99
| 12,99<ref name=RECONS />
| 15.85
| 15,85<ref name=RECONS />
| ~2600
|-
|-
| 7
| style="background-color: #CCC;" | 7
| colspan="2" style="background-color: #CCC;" | [[Ross 154]] (V1216 Sagittarii)
| colspan="2" | [[Ross 154|Ross&nbsp;154]] (V1216&nbsp;Sagittarii)
| 11
| style="background-color: #F99;" | M3.5Ve
| style="background: {{estrela-cor|M}};" | M3.5Ve
| 10.43
| 10,43<ref name=RECONS />
| 13.07
| 13,07<ref name=RECONS />
| ~2700
| {{RA|18|49|49}}
| {{RA|18|49|49,4}}
| {{DEC|−23|50|11}}
| {{DEC|−23|50|10}}
| align=left | 336,90(178)<ref name="Y"/><ref name="H"/>
| 0.336 9(1 8)″
| 9.6811(512)
| 9,6813(512)
|
|-
|-
| 8
| style="background-color: #CCC;" | 8
| colspan="2" style="background-color: #CCC;" | [[Ross 248]] (HH Andromedae)
| colspan="2" | [[Ross 248|Ross&nbsp;248]] (HH&nbsp;Andromedae)
| 12
| style="background-color: #F99;" | M5.5Ve
| style="background: {{estrela-cor|M}};" | M5.5Ve
| 12.29
| 12,29<ref name=RECONS />
| 14.79
| 14,79<ref name=RECONS />
| -
| {{RA|23|41|54}}
| {{RA|23|41|54,7}}
| {{DEC|+44|09|32}}
| {{DEC|+44|10|30}}
| align=left | 316,00(110)<ref name="Y"/>
| 0.316 0(1 1)″
| 10.321(36)
| 10,322(36)
|
|-
|-
| 9
| 9
| colspan="2" | [[Epsilon Eridani]] (BD-09°697)
| colspan="2" | [[Epsilon Eridani|Epsilon&nbsp;Eridani]] (BD−09°697)
| 13
| style="background-color: #FC9;" | K2V
| style="background: {{estrela-cor|K}};" | [[anã laranja|K2V]]<ref name=RECONS />
| 3.73
| style="background: lightblue;" | 3,73<ref name=RECONS />
| 6.19
| 6,19<ref name=RECONS />
| 5100
| {{RA|03|32|56}}
| {{RA|03|32|55,8}}
| {{DEC|−09|27|30}}
| {{DEC|−09|27|30}}
|align=left | 309,99(079)<ref name="Y"/><ref name="H"/>
| 0.310 0(0 8)″
| 10.522(27)
| 10,522(27)
| acredita-se que tem dois planetas<ref>{{citation | display-authors=1| last1=Janson | first1=M.| last2=Reffert | first2=S.| last3=Brandner | first3=W.| last4=Henning | first4=T.| last5=Lenzen | first5=R.| last6=Hippler | first6=S.| title=A comprehensive examination of the ε Eridani system. Verification of a 4 micron narrow-band high-contrast imaging approach for planet searches | journal=Astronomy and Astrophysics | volume=488 | issue=2 | pages=771–780 | date=setembro de 2008 | bibcode=2008A&A...488..771J | doi=10.1051/0004-6361:200809984 | arxiv=0807.0301 }}</ref>
|-
|-
| 10
| style="background-color: #CCC;" | 10
| colspan="2" style="background-color: #CCC;" | [[Lacaille 9352]] (CD-36°15693)
| colspan="2" | [[Lacaille 9352|Lacaille&nbsp;9352]] (CD−36°15693)
| 14
| style="background-color: #F99;" | M1.5Ve
| style="background: {{estrela-cor|M}};" | M1.5Ve
| 7.34
| 7,34<ref name=RECONS />
| 9.75
| 9,75<ref name=RECONS />
| 3340
| {{RA|23|05|42}}
| {{RA|23|05|52,0}}
| {{DEC|−35|51|11}}
| {{DEC|−35|51|11}}
| align=left | 303,64(087)<ref name="Y"/><ref name="H"/>
| 0.303 6(0 9)″
| 10.742(31)
| 10,742(31)
|
|-
|-
| 11
| style="background-color: #CCC;" | 11
| colspan="2" style="background-color: #CCC;" | [[Ross 128]] (FI Virginis)
| colspan="2" | [[Ross 128|Ross&nbsp;128]] (FI&nbsp;Virginis)
| 15
| style="background-color: #F99;" | M4.0Vn
| style="background: {{estrela-cor|M}};" | M4.0Vn
| 11.13
| 11,13<ref name=RECONS />
| 13.51
| 13,51<ref name=RECONS />
| -
| {{RA|11|47|45}}
| {{RA|11|47|44,4}}
| {{DEC|+00|48|17}}
| {{DEC|+00|48|16}}
| align=left | 298,72(135)<ref name="Y"/><ref name="H"/>
| 0.298 7(1 4)″
| 10.918(50)
| 10,919(49)
|
|-
|-
| rowspan="3" style="background-color: #CCC;" | 12
| rowspan="3" | 12
| rowspan="3" style="background-color: #CCC;" | [[EZ Aquarii]]
| rowspan="3" | [[EZ Aquarii|EZ&nbsp;Aquarii]]<br>(Gliese&nbsp;866, Luyten&nbsp;789-6)
| EZ&nbsp;Aquarii&nbsp;A
| style="background-color: #CCC;" | EZ Aquarii (L 0789-006)
| 16
<!---
| style="background: {{estrela-cor|M}};" | M5.0Ve
It is also known as
| 13,33<ref name=RECONS />
[[Henry-Lee Giclas|G]] 156-031,
| 15,64<ref name=RECONS />
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 5475.00,
| rowspan="3" | {{RA|22|38|33,4}}
[[Luyten Half-Second catalogue|LHS]] 68 and
| rowspan="3" | {{DEC|−15|18|07}}
Luyten 0789-006.
| rowspan="3" align=left | 289,50(440)<ref name="Y"/>
--->| style="background-color: #F99;" | M5.0Ve
| rowspan="3" | 11,266(171)
| 13.33
| rowspan="3" |
| 15.64
| -
| rowspan="3" | {{RA|22|38|34}}
| rowspan="3" | {{DEC|−15|18|02}}
| rowspan="3" | 0.289 5(4 4)″
| rowspan="3" | 11.266(172)
|-
|-
| EZ&nbsp;Aquarii&nbsp;B
| style="background-color: #CCC;" | Gl 866 B
| 16
| style="background-color: #F99;" | M?
| style="background: {{estrela-cor|M}};" | M?
| 13.27
| 13,27<ref name=RECONS />
| 15.58
| 15,58<ref name=RECONS />
| -
|-
|-
| EZ&nbsp;Aquarii&nbsp;C
| style="background-color: #CCC;" | Gl 866 C
| 16
| style="background-color: #F99;" | M?
| style="background: {{estrela-cor|M}};" | M?
| 14.03
| 14,03<ref name=RECONS />
| 16.34
| 16,34<ref name=RECONS />
| -
|-
|-
| rowspan="2" | 13
| rowspan="2" | 13
| rowspan="2" | [[Procyon (estrela)|Procyon]]
| rowspan="2" | [[Procyon]]<br>(α&nbsp;Canis&nbsp;Minoris)
| Procyon A (α Canis Minoris)
| Procyon&nbsp;A
|19
| bgcolor="ffffcc" | F5V-IV
| style="background: {{estrela-cor|F}}" | F5V-IV<ref name=RECONS />
| 0.38
| style="background: lightblue;" | 0,38<ref name=RECONS />
| 2.66
| 2,66<ref name=RECONS />
| -
| rowspan="2" | {{RA|07|39|18}}
| rowspan="2" | {{RA|07|39|18,1}}
| rowspan="2" | {{DEC|+05|13|30}}
| rowspan="2" | {{DEC|+05|13|30}}
| rowspan="2" | 0.286 1(0 9)″
| rowspan="2" align=left | 286,05(081)<ref name="Y"/><ref name="H"/>
| rowspan="2" | 11.402(33)
| rowspan="2" | 11,402(32)
| rowspan="2" |
|-
|-
| Procyon&nbsp;B
| style="background-color: #CCC;" | Procyon B
| 19
| bgcolor="F0F0F0" | [[Anã branca|DA]]
| style="background: #F0F0F0" | [[Anã branca|DA]]<ref name=RECONS />
| 10.7
| 10,70<ref name=RECONS />
| 12.98
| 12,98<ref name=RECONS />
| -
|-
|-
| rowspan="2" | 14
| rowspan="2" | 14
| rowspan="2" | [[61 Cygni]]
| rowspan="2" | [[61 Cygni|61&nbsp;Cygni]]
| 61 Cygni A (BD+38°4343)
| 61&nbsp;Cygni&nbsp;A (BD+38°4343)
|21
| style="background-color: #FC9;" | K5.0V <!--previous: K3.5Ve-->
| style="background: {{estrela-cor|K}};" | [[anã laranja|K5.0V]]<ref name=RECONS /> <!--previous: K3.5Ve-->
| 5.21
| style="background: lightblue;" | 5,21<ref name=RECONS />
| 7.49
| 7,49<ref name=RECONS />
| -
| rowspan="2" | {{RA|21|08|52}}
| {{RA|21|06|53,9}}
| rowspan="2" | {{DEC|+38|56|51}}
| {{DEC|+38|44|58}}
| rowspan="2" | 0.286 0(0 6)″
| rowspan="2" align=left | 286,04(056)<ref name="Y"/><ref name="H"/>
| rowspan="2" | 11.402(23)
| rowspan="2" | 11,403(22)
| rowspan="2" | primeira estrela (além do Sol) a ter sua distância medida<ref>{{cite journal | last=Bessel | first=F. W. | title=Bestimmung der Entfernung des 61sten Sterns des Schwans. Von Herrn Geheimen - Rath und Ritter Bessel | journal=Astronomische Nachrichten | year=1839 | volume=16 | issue=5-6 | pages=65 | language=German | bibcode=1839AN.....16...65B | quote=(page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist | doi=10.1002/asna.18390160502 }} A parallax of 313.6 mas yields a distance of 10.4 light years</ref>
|-
|-
| 61 Cygni B (BD+38°4344)
| 61&nbsp;Cygni&nbsp;B (BD+38°4344)
|21
| style="background-color: #FC9;" | K7.0V <!--previous: K4.7Ve-->
| style="background: {{estrela-cor|K}};" | [[anã laranja|K7.0V]]<ref name=RECONS /> <!--previous: K4.7Ve-->
| 6.03
| style="background: lightblue;" | 6,03<ref name=RECONS />
| 8.31
| 8,31<ref name=RECONS />
| -
| {{RA|21|06|55,3}}
| {{DEC|+38|44|31}}
|-
|-
| rowspan="2" style="background-color: #CCC;" | 15
| rowspan="2" | 15
| rowspan="2" style="background-color: #CCC;" | [[Struve 2398]]
| rowspan="2" | [[Struve 2398|Struve&nbsp;2398]]<br>(Gliese&nbsp;725, BD+59°1915)
| Struve&nbsp;2398&nbsp;A (HD&nbsp;173739)
| style="background-color: #CCC;" | Struve 2398 A (GJ 725 A, BD+59°1915)
| 23
<!---
| style="background: {{estrela-cor|M}};" | M3.0V<ref name=RECONS />
It is also known as
| 8,90<ref name=RECONS />
[[Henry Draper catalogue|HD]] 173739,
| 11,16<ref name=RECONS />
[[Bonner Durchmusterung|BD]]+59°1915,
| {{RA|18|42|46,7}}
[[Henry-Lee Giclas|G]] 227-046,
| {{DEC|+59|37|49}}
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 4330.00A,
| rowspan="2" align=left | 283,00(169)<ref name="Y"/><ref name="H"/>
[[Luyten Half-Second catalogue|LHS]] 58 and
| rowspan="2" | 11,525(69)
[[Alexander N. Vyssotsky|Vyssotsky]] 184.
| rowspan="2" |
[[Category:Draco constellation]]
--->| style="background-color: #F99;" | M3.0V
| 8.90
| 11.16
| -
| rowspan="2" | {{RA|18|42|47}}
| rowspan="2" | {{DEC|+59|37|50}}
| rowspan="2" | 0.283 0(1 7)″
| rowspan="2" | 11.525(69)
|-
|-
| style="background-color: #CCC;" | Struve 2398 B (HD 173740)
| Struve&nbsp;2398&nbsp;B (HD&nbsp;173740)
| 23
<!---
| style="background: {{estrela-cor|M}};" | M3.5V<ref name=RECONS />
It is also known as
| 9,69<ref name=RECONS />
[[Henry Draper catalogue|HD]] 173740,
| 11,95<ref name=RECONS />
[[Henry-Lee Giclas|G]] 227-047,
| {{RA|18|42|46,9}}
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 4330.00B and
| {{DEC|+59|37|37}}
[[Luyten Half-Second catalogue|LHS]] 59.
[[Category:Draco constellation]]
--->| style="background-color: #F99;" | M3.5V
| 9.69
| 11.95
| -
|-
|-
| rowspan="2" style="background-color: #CCC;" | 16
| rowspan="2" | 16
| rowspan="2" style="background-color: #CCC;" | [[Groombridge 34]]
| rowspan="2" | [[Groombridge 34|Groombridge&nbsp;34]]<br>(Gliese&nbsp;15)
| style="background-color: #CCC;" | Gl 15 A (GX Andromedae)
| Groombridge&nbsp;34&nbsp;A (GX&nbsp;Andromedae)
| 25
<!---
| style="background: {{estrela-cor|M}};" | M1.5V<ref name=RECONS /> <!--previous: M3.0V-->
It is also known as
| 8,08<ref name=RECONS />
[[Henry Draper catalogue|HD]] 1326,
| 10,32<ref name=RECONS />
[[Bonner Durchmusterung|BD]]+43°44,
| rowspan="2" | {{RA|0|18|22,9}}
[[Henry-Lee Giclas|G]] 171-047,
| rowspan="2" | {{DEC|+44|01|23}}
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 49.00A,
| rowspan="2" align=left | 280,59(095)<ref name="Y"/><ref name="H"/>
[[Luyten Half-Second catalogue|LHS]] 3 and
| rowspan="2" | 11,624(39)
[[Alexander N. Vyssotsky|Vyssotsky]] 85.
| rowspan="2" |
--->| style="background-color: #F99;" | M1.5V <!--previous: M3.0V-->
| 8.08
| 10.32
| -
| rowspan="2" | {{RA|0|18|24}}
| rowspan="2" | {{DEC|+44|1|24}}
| rowspan="2" | 0.280 6(1 0)″
| rowspan="2" | 11.624(40)
|-
|-
| style="background-color: #CCC;" | Gl 15 B (GQ Andromedae)
| Groombridge&nbsp;34&nbsp;B (GQ&nbsp;Andromedae)
| 25
<!---
| style="background: {{estrela-cor|M}};" | M3.5V<ref name=RECONS />
It is also known as
| 11,06<ref name=RECONS />
[[Henry-Lee Giclas|G]] 171-048 and
| 13,30<ref name=RECONS />
[[Luyten Half-Second catalogue|LHS]] 4.
--->| style="background-color: #F99;" | M3.5V
| 11.06
| 13.30
| -
|-
|-
| 17
| rowspan="3" | 17
| colspan="2" | [[Epsilon Indi]] (CP−57°10015)
| rowspan="3" | [[Epsilon Indi|Epsilon&nbsp;Indi]]<br>(CPD−57°10015)
| Epsilon Indi A
| style="background-color: #FC9;" | K5Ve
|27
| 4.69
| style="background: {{estrela-cor|K}};" | [[anã laranja|K5Ve]]<ref name=RECONS />
| 6.89
| style="background: lightblue;" | 4,69<ref name=RECONS />
| -
| 6,89<ref name=RECONS />
| {{RA|22|03|22}}
| {{RA|22|03|21,7}}
| {{DEC|−56|47|10}}
| {{DEC|−56|47|10}}
| rowspan="3" align=left | 275,84(069)<ref name="Y"/><ref name="H"/>
| 0.275 8(0 7)″
| 11.824(30)
| rowspan="3" | 11,824(30)
| rowspan="3" |
|-
|-
| style="background-color: #CCC;" | 18
| style="background: #C67B30"| Epsilon&nbsp;Indi&nbsp;Ba
| 27
| colspan="2" style="background-color: #CCC;" | [[DX Cancri]] (G051-015)
| style="background: {{estrela-cor|T}};" | [[Anã marrom|T1.0V]]
<!---
| 12,3 J<ref name="DwarfArchives"> {{cite web
It is also known as
|title=DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs
[[Henry-Lee Giclas|G]] 051-015,
|publisher=caltech.edu
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 2016.01 and
|author=Chris Gelino, [[J. Davy Kirkpatrick|Davy Kirkpatrick]], Adam Burgasser
[[Luyten Half-Second catalogue|LHS]] 248.
|url=http://ldwarf.ipac.caltech.edu/archive/version5/viewlist.php?table=ltdwarf&format=text
--->| style="background-color: #F99;" | M6.5Ve
|accessdate=10/06/2012}} [http://spider.ipac.caltech.edu/staff/davy/ARCHIVE/index.shtml (main page)]</ref>
| 14.78
| 16.98
|
| rowspan="2" | {{RA|22|04|10,5}}
| -
| {{RA|08|29|50}}
| rowspan="2" | {{DEC|−56|46|58}}
|-
| style="background: #C67B30"| Epsilon&nbsp;Indi&nbsp;Bb
| 27
| style="background: {{estrela-cor|T}};" | [[Anã marrom|T6.0V]]
| 13,2 J<ref name="DwarfArchives"/>
|
|-
| 18
| colspan="2" | [[DX Cancri|DX&nbsp;Cancri]] (G&nbsp;51-15)
| 30
| style="background: {{estrela-cor|M}};" | M6.5Ve
| 14,78<ref name=RECONS />
| 16,98<ref name=RECONS />
| {{RA|08|29|49,5}}
| {{DEC|+26|46|37}}
| {{DEC|+26|46|37}}
| align=left | 275,80(300)<ref name=Y />
| 0.275 8(3 0)″
| 11.826(129)
| 11,826(129)
|
|-
|-
| 19
| 19
| colspan="2" | [[Tau Ceti]] (BD−16°295)
| colspan="2" | [[Tau Ceti|Tau&nbsp;Ceti]] (BD−16°295)
| 31
| style="background-color: #FF9;" | G8Vp
| style="background: {{estrela-cor|G}};" | [[anã amarela|G8Vp]]<ref name=RECONS />
| 3.49
|style="background: lightblue;" | 3,49<ref name=RECONS />
| 5.68
| 5,68<ref name=RECONS />
| -
| {{RA|01|44|04}}
| {{RA|01|44|04,1}}
| {{DEC|−15|56|15}}
| {{DEC|−15|56|15}}
| align=left | 274,39(076)<ref name="Y"/><ref name="H"/>
| 0.274 4(0 8)″
| 11.887(33)
| 11,887(33)
|
|-
|-
| 20
| style="background-color: #CCC;" | 20
| colspan="2" style="background-color: #CCC;" | [[GJ 1061]] (LHS 1565)
| colspan="2" | [[GJ 1061]] (LHS&nbsp;1565)
| 32
| style="background-color: #F99;" | M5.5V
| style="background: {{estrela-cor|M}};" | M5.5V<ref name=RECONS />
| 13.03
| 13,09<ref name=RECONS />
| 15.19
| 15,26<ref name=RECONS />
| -
| {{RA|03|35|57}}
| {{RA|03|35|59,7}}
| {{DEC|−44|30|46}}
| {{DEC|−44|30|45}}
| align=left | 272,01(130)<ref name="recent">Systems with their first accurate trigonometric parallaxes measured by RECONS</ref>
| style="color: red;" | 0.272 0(1 3)″
| style="color: red;" | 11.991(58)
| 11,991(57)
| <ref name=henry1997>[http://adsabs.harvard.edu/abs/1997AJ....114..388H The solar neighborhood IV: discovery of the twentieth nearest star], Todd J. Henry, Philip A. Ianna, J. Davy Kirkpatrick, Hartmut Jahreiss, ''The Astronomical Journal'' '''114''', #1 (julho de 1997), pp. 388&ndash;395. {{doi|10.1086/118482}}</ref><ref name=henry2006>[http://adsabs.harvard.edu/abs/2006AJ....132.2360H The Solar Neighborhood. XVII. Parallax Results from the CTIOPI 0.9 m Program: 20 New Members of the RECONS 10 Parsec Sample], Todd J. Henry, Wei-Chun Jao, John P. Subasavage, Thomas D. Beaulieu, Philip A. Ianna, Edgardo Costa, René A. Méndez, ''The Astronomical Journal'' '''132''', #6 (dezembro de 2006), pp. 2360&ndash;2371. {{doi|10.1086/508233}}</ref>
|-
|-
| 21
| style="background-color: #CCC;" | 21
| colspan="2" style="background-color: #CCC;" | [[YZ Ceti]] (LHS 138)
| colspan="2" | [[YZ Ceti|YZ&nbsp;Ceti]] (LHS&nbsp;138)
| 33
<!---
| style="background: {{estrela-cor|M}};" | M4.5V<ref name=RECONS />
It is also known as
| 12,02<ref name=RECONS />
[[Henry-Lee Giclas|G]] 268-135,
| 14,17<ref name=RECONS />
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 248.01,
| {{RA|01|12|30,6}}
[[Luyten Half-Second catalogue|LHS]] 138,
| {{DEC|−16|59|56}}
Luyten 0725-032 and
| align=left | 268,84(295)<ref name="Y"/><ref name="H"/>
[[Luyten Two-Tenths catalogue|LTT]] 670.
| 12,132(133)
--->| style="background-color: #F99;" | M4.5V
|
| 12.02
| 14.17
| -
| {{RA|01|12|31}}
| {{DEC|−16|59|57}}
| 0.268 8(3 0)″
| 12.132(14)
|-
|-
| 22
| style="background-color: #CCC;" | 22
| colspan="2" style="background-color: #CCC;" | [[Estrela de Luyten]] (BD+05°1668)
| colspan="2" | [[Estrela de Luyten]] (BD+05°1668)
| 34
| style="background-color: #F99;" | M3.5Vn
| style="background: {{estrela-cor|M}};" | M3.5Vn
| 9.86
| 9,86<ref name=RECONS />
| 11.97
| 11,97<ref name=RECONS />
| -
| {{RA|07|27|25}}
| {{RA|07|27|24,5}}
| {{DEC|+05|13|33}}
| {{DEC|+05|13|33}}
| align=left | 263,76(125)<ref name="Y"/><ref name="H"/>
| 0.263 8(1 3)″
| 12.366(59)
| 12,366(59)
|
|-
|-
| 23
| style="background-color: #CCC;" | 23
| colspan="2" style="background-color: #CCC;" | [[Estrela de Teegarden]] (SO025300.5+165258)
| style="background: #C67B30" colspan="2" | [[Estrela de Teegarden]] (SO025300.5+165258)
| 35
| style="background-color: #F99;" | M6.5V
| style="background: {{estrela-cor|M}};" | M6.5V
| 15.40
| 15,14<ref name=RECONS />
| 18.50
| 17,22<ref name=RECONS />
| -
| {{RA|02|53|01}}
| {{RA|02|53|00,9}}
| {{DEC|+16|52|58}}
| {{DEC|+16|52|53}}
| align=left | 260,63(269)<ref name=recent />
| style="color: red;" | 0.260 6(2 7)″
| style="color: red;" | 12.514(130)
| 12,514(129)
| <ref name=henry2006 />
|-
|-
| style="background-color: #CCC;" | 24
| rowspan="2" | 24
| colspan="2" style="background-color: #CCC;" | [[SCR 1845-6357]]
| rowspan="2" | [[SCR 1845-6357|SCR&nbsp;1845-6357]]
| SCR&nbsp;1845-6357&nbsp;A
| style="background-color: #F99;" | M8.5V
| 17.39
| 36
| style="background: {{estrela-cor|M}};" | M8.5V<ref name=RECONS />
| 19.41
| -
| 17,39
| 19,41
| {{RA|18|45|03}}
| {{RA|18|45|05,3}}
| {{DEC|−63|57|48}}
| {{DEC|−63|57|48}}
| rowspan=2 align=left | 259,45(111)<ref name="recent"/>
| style="color: red;" | 0.259 5(1 2)″
| style="color: red;" | 12.571(54)
| rowspan=2 | 12,571(54)
| rowspan=2 | <ref name=henry2006 />
|-
|-
| style="background-color: #CCC;" | 25
| style="background: #C67B30"| SCR&nbsp;1845-6357&nbsp;B
| 36
| colspan="2" style="background-color: #CCC;" | [[Estrela de Kapteyn]] (CD−45°1841)
| style="background: {{estrela-cor|T}};" | [[Anã marrom|T6]]<ref name=nearmt>[http://adsabs.harvard.edu/abs/2007A%26A...471..655K The very nearby M/T dwarf binary SCR 1845-6357], Markus Kasper, Beth A. Biller, Adam Burrows, Wolfgang Brandner, Jano Budaj, and Laird M. Close, ''Astronomy and Astrophysics'' '''471''', #2 (agosto de 2007), pp. 655&ndash;659. {{doi|10.1051/0004-6361:20077881}}</ref>
| style="background-color: #F99;" | M1.5V <!--previous: sdM0VI-->
| 13,3 J<ref name="DwarfArchives"/>
| 8.84
| 10.87
|
| {{RA|18|45|02,6}}
| -
| {{RA|05|11|41}}
| {{DEC|−63|57|52}}
|-
| 25
| colspan="2" | [[Estrela de Kapteyn]] (CD−45°1841)
| 38
| style="background: {{estrela-cor|M}};" | M1.5V<ref name=RECONS /> <!--previous: sdM0VI-->
| 8,84<ref name=RECONS />
| 10,87<ref name=RECONS />
| {{RA|05|11|40,6}}
| {{DEC|−45|01|06}}
| {{DEC|−45|01|06}}
| align=left | 255,27(086)<ref name="Y"/><ref name="H"/>
| 0.255 3(0 9)″
| 12.777(44)
| 12,777(43)
|
|-
|-
| 26
| style="background-color: #CCC;" | 26
| colspan="2" style="background-color: #CCC;" | [[Lacaille 8760]] ([[AX Microscopii]])
| colspan="2" | [[Lacaille 8760|Lacaille&nbsp;8760]] (AX&nbsp;Microscopii)
| 39
<!---
| style="background: {{estrela-cor|M}};" | M0.0V<ref name=RECONS /> <!--previous: M2Ve-->
It is also known as
| 6,67<ref name=RECONS />
[[Henry Draper catalogue|HD]] 202560,
| 8,69<ref name=RECONS />
[[Cordoba Durchmusterung|CD]]−39°14192,
| {{RA|21|17|15,3}}
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 5117.00,
[[Luyten Half-Second catalogue|LHS]] 66 and UGPMF 518.
--->| style="background-color: #F99;" | M0.0V <!--previous: M2Ve-->
| 6.67
| 8.69
| -
| {{RA|21|17|15}}
| {{DEC|−38|52|03}}
| {{DEC|−38|52|03}}
| align=left | 253,43(112)<ref name="Y"/><ref name="H"/>
| 0.253 4(1 2)″
| 12.870(57)
| 12,870(57)
|
|-
|-
| rowspan="2" style="background-color: #CCC;" | 27
| rowspan="2" | 27
| rowspan="2" style="background-color: #CCC;" | [[Kruger 60]]
| rowspan="2" | [[Kruger 60|Kruger&nbsp;60]]<br>(BD+56°2783)
| Kruger&nbsp;60&nbsp;A
| style="background-color: #CCC;" | Kruger 60 A (BD+56°2783)
| 40
| style="background-color: #F99;" | M3.0V
| style="background: {{estrela-cor|M}};" | M3.0V<ref name=RECONS />
| 9.79
| 9,79<ref name=RECONS />
| 11.76
| 11,76<ref name=RECONS />
| -
| rowspan="2" | {{RA|22|28|00}}
| rowspan="2" | {{RA|22|27|59,5}}
| rowspan="2" | {{DEC|+57|41|45}}
| rowspan="2" | {{DEC|+57|41|45}}
| rowspan="2" | 0.248 1(1 4)″
| rowspan="2" align=left | 248,06(139)<ref name="Y"/><ref name="S"/>
| rowspan="2" | 13.148(74)
| rowspan="2" | 13,149(74)
| rowspan="2" |
|-
|-
| style="background-color: #CCC;" | Kruger 60 B (DO Cephei)
| Kruger&nbsp;60&nbsp;B (DO&nbsp;Cephei)
| 40
| style="background-color: #F99;" | M4.0V
| style="background: {{estrela-cor|M}};" | M4.0V<ref name=RECONS />
| 11.41
| 11,41<ref name=RECONS />
| 13.38
| 13,38<ref name=RECONS />
| -
|-
|-
| 28
| style="background-color: #CCC;" | 28
| colspan="2" style="background-color: #CCC;" | [[DEN 1048-3956]]
| style="background: #C67B30" colspan="2" | [[DEN 1048-3956|DEN&nbsp;1048-3956]]
| 42
| style="background-color: #F99;" | M8.5 V
| style="background: {{estrela-cor|M}};" | M8.5V<ref name=RECONS />
| 17.39
| 17,39<ref name=RECONS />
| 19.37
| 19,37<ref name=RECONS />
| -
| {{RA|10|48|15}}
| {{RA|10|48|14,7}}
| {{DEC|−39|56|06}}
| {{DEC|−39|56|06}}
| align=left | 247,71(155)<ref name="recent"/>
| 0.247 7(1 6)″
| 13.167(83)
| 13,167(82)
| <ref>[http://adsabs.harvard.edu/abs/2005AJ....129.1954J The Solar Neighborhood. XIII. Parallax Results from the CTIOPI 0.9 Meter Program: Stars with μ >= 1.0" yr<sup>-1</sup> (Motion sample)], Wei-Chun Jao, Todd J. Henry, John P. Subasavage, Misty A. Brown, Philip A. Ianna, Jennifer L. Bartlett, Edgardo Costa, René A. Méndez, ''The Astronomical Journal'' '''129''', #4 (abril de 2005), pp. 1954&ndash;1967. {{doi|10.1086/428489}}</ref><ref name=costa2005>[http://adsabs.harvard.edu/abs/2005AJ....130..337C The Solar Neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation&mdash;First Results from the 1.5 m Telescope Program], Edgardo Costa, René A. Méndez, W.-C. Jao, Todd J. Henry, John P. Subasavage, Misty A. Brown, Philip A. Ianna, and Jennifer Bartlett, ''The Astronomical Journal'' '''130''', #1 (julho de 2005), pp. 337&ndash;349. {{doi|10.1086/430473}}</ref>
|-
|-
| 29
| rowspan="2" style="background-color: #CCC;" | 29
| rowspan="2" style="background-color: #CCC;" | [[Ross 614]]
| style="background: #C67B30" colspan="2" |[[UGPS J072227.51-054031.2|UGPS 0722-05]]
| 43
| style="background-color: #CCC;" | Ross 614 (LHS 1849)
| style="background: {{estrela-cor|T}};" | T9<ref name=RECONS /> <!--previous: M2Ve-->
<!---
| 16,52 J<ref>{{Cite arxiv | eprint=1004.0317v2 | author1=Lucas | author2=Tinney | author3=Ben Burningham | author4=Leggett | author5=Pinfield | author6=Richard Smart | author7=Jones | author8=Federico Marocco | author9=Barber | title=The discovery of a very cool, very nearby brown dwarf in the Galactic plane | class=astro-ph.SR | year=2010 }}</ref>
It is also known as
|
[[Henry-Lee Giclas|G]] 106-049,
| {{RA|07|22|27,3}}
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 1509.00 and
| {{DEC|–05|40|30}}
[[Luyten Half-Second catalogue|LHS]] 1849.
| align=left | 246
--->| style="background-color: #F99;" | M4.5V
| 11.15
| 13,259
|<ref name="Lucas2010v2">{{cite arXiv
| 13.09
|last=Lucas |first=Philip W.
| -
|coauthors=Tinney; Burningham; Leggett; Pinfield; Smart; et al.
| rowspan="2" | {{RA|06|29|23}}
|title=Discovery of a very cool brown dwarf amongst the ten nearest stars to the Solar System
|year=2010
|eprint=1004.0317
|version=v1
|class=astro-ph.SR}}</ref>
|-
| rowspan="2" | 30
| rowspan="2" | [[Ross 614|Ross&nbsp;614]]<br>(V577&nbsp;Monocerotis, Gliese 234)
| Ross&nbsp;614A (LHS&nbsp;1849)
| 44
| style="background: {{estrela-cor|M}};" | M4.5V<ref name=RECONS/>
| 11,15<ref name=RECONS />
| 13,09<ref name=RECONS />
| rowspan="2" | {{RA|06|29|23,4}}
| rowspan="2" | {{DEC|−02|48|50}}
| rowspan="2" | {{DEC|−02|48|50}}
| rowspan="2" | 0.244 3(2 1)″
| rowspan="2" align=left | 244,34(201)<ref name="Y"/><ref name="S"/>
| rowspan="2" | 13.348(110)
| rowspan="2" | 13,349(110)
| rowspan="2" |
|-
| Ross&nbsp;614B (LHS&nbsp;1850)
| 44
| style="background: {{estrela-cor|M}};" | M5.5V
| 14,23<ref name=RECONS />
| 16,17<ref name=RECONS />
|-
| 31
| style="background: #C67B30" colspan="2" | [[WISE 1541-2250]]
| 46
| style="background: {{estrela-cor|Y}};" | [[Anã marrom|Y0.5]]
| 20,74 J<ref name="Kirkpatrick2012v1"/>
|
|| {{RA|15|41|51,57}}
|| {{DEC|−22|50|25}}
| 238 <ref name="Kirkpatrick2012v1" />
| 13,704<ref name="Kirkpatrick2012v1">{{cite arXiv |last=Kirkpatrick |first=J. Davy |coauthors=Gelino; Cushing; Mace; Griffith; Skrutskie; Marsh; Wright; Eisenhardt; McLean; Mainzer; Burgasser; Tinney; Parker; Salter |title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf mass Function |year=2012 |eprint=1205.2122 |version=v1 |class=astro-ph.SR}}</ref>
|
|-
|-
| 32
| style="background-color: #CCC;" | Gl 234 B (V577 Monocerotis)
| style="background: #C67B30" colspan="2" | [[WISE 0350-5658]]
<!---
| 47
It is also known as
| style="background: {{estrela-cor|Y}};" | [[Anã marrom|Y1]]
[[Luyten Half-Second catalogue|LHS]] 1850.
| >22,8 J<ref name="Kirkpatrick2012v1"/>
--->| style="background-color: #F99;" | M5.5V
| 14.23
|
|| {{RA|03|50}}
| 16.17
|| {{DEC|−56|58}}
| -
| 238 <ref name="Kirkpatrick2012v1" />
| 13,704<ref name="Kirkpatrick2012v1">{{cite arXiv |last=Kirkpatrick |first=J. Davy |coauthors=Gelino; Cushing; Mace; Griffith; Skrutskie; Marsh; Wright; Eisenhardt; McLean; Mainzer; Burgasser; Tinney; Parker; Salter |title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf mass Function |year=2012 |eprint=1205.2122 |version=v1 |class=astro-ph.SR}}</ref>
|
|-
|-
| 33
| style="background-color: #CCC;" | 30
| colspan="2" style="background-color: #CCC;" | [[Gl 628]] (Wolf 1061, BD−12°4523)
| colspan="2" | [[Wolf&nbsp;1061]] (Gliese 628, BD−12°4523)
| 48
<!---
| style="background: {{estrela-cor|M}};" | M3.0V<ref name=RECONS />
It is also known as
| 10,07<ref name=RECONS />
[[Bonner Durchmusterung|BD]]−12°4523,
| 11,93<ref name=RECONS />
[[Henry-Lee Giclas|G]] 153-058,
| {{RA|16|30|18,1}}
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 3746.00,
[[Luyten Half-Second catalogue|LHS]] 419 and
[[Alexander N. Vyssotsky|Vyssotsky]] 164.
[[Category:Ophiuchus constellation]]
--->| style="background-color: #F99;" | M3.0V
| 10.07
| 11.93
| -
| {{RA|16|30|18}}
| {{DEC|−12|39|45}}
| {{DEC|−12|39|45}}
| align=left | 236,01(167)<ref name="Y"/><ref name="H"/>
| 0.236 0(1 7)″
| 13.820(98)
| 13,820(98)
|
|-
|-
| 34
| style="background-color: #CCC;" | 31
| colspan="2" style="background-color: #CCC;" | [[Estrela de Van Maanen]] (Gl 35, LHS 7)
| colspan="2" | [[Estrela de van Maanen]] (Gliese 35, LHS&nbsp;7)
| 49
| bgcolor="F0F0F0" | [[Anã branca|DZ7]]
| style="background: #F0F0F0" | [[Anã branca|DZ7]]<ref name=RECONS />
| 12.38
| 12,38<ref name=RECONS />
| 14.21
| 14,21<ref name=RECONS />
| -
| {{RA|00|49|10}}
| {{RA|00|49|09,9}}
| {{DEC|+05|23|19}}
| {{DEC|+05|23|19}}
| align=left | 231,88(179)<ref name="Y"/><ref name="H"/>
| 0.231 9(1 8)″
| 14.066(109)
| 14,066(109)
|
|-
|-
| 35
| style="background-color: #CCC;" | 32
| colspan="2" style="background-color: #CCC;" | [[Gl 1]] (CD−37°15492)
| colspan="2" | [[Gliese 1]] (CD−37°15492)
| 50
<!---
| style="background: {{estrela-cor|M}};" | M3.0V<ref name=RECONS />
It is also known as
| 8,55<ref name=RECONS />
[[Henry Draper catalogue|HD]] 225213,
| 10,35<ref name=RECONS />
[[Cordoba Durchmusterung|CD]]-37°15492,
| {{RA|00|05|24,4}}
[[Henry-Lee Giclas|G]] 267-025,
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 5817.00 and
[[Luyten Half-Second catalogue|LHS]] 1.
[[Category:Sculptor constellation]]
--->| style="background-color: #F99;" | M3.0V
| 8.55
| 10.35
| -
| {{RA|00|05|24}}
| {{DEC|−37|21|27}}
| {{DEC|−37|21|27}}
| align=left | 229,20(107)<ref name="Y"/><ref name="H"/>
| 0.229 2(1 1)″
| 14.230(67)
| 14,231(66)
|
|-
|-
| rowspan="2" style="background-color: #CCC;" | 33
| rowspan="2" | 36
| rowspan="2" style="background-color: #CCC;" | [[Wolf 424]]
| rowspan="2" | [[Wolf 424|Wolf&nbsp;424]]<br>(FL&nbsp;Virginis, LHS&nbsp;333, Gliese 473)
| Wolf&nbsp;424&nbsp;A
| style="background-color: #CCC;" | Wolf 424 A (LHS 333)
| 51
<!---
| style="background: {{estrela-cor|M}};" | M5.5Ve
It is also known as
| 13,18<ref name=RECONS />
[[Henry-Lee Giclas|G]] 012-043,
| 14,97<ref name=RECONS />
[[General Catalogue of Trigonometric Parallaxes|GCTP]] 2890.00A and
| rowspan="2" | {{RA|12|33|17,2}}
[[Luyten Half-Second catalogue|LHS]] 333.
--->| style="background-color: #F99;" | M5.5Ve
| 13.18
| 14.97
| -
| rowspan="2" | {{RA|17|33|17}}
| rowspan="2" | {{DEC|+09|01|15}}
| rowspan="2" | {{DEC|+09|01|15}}
| rowspan="2" | 0.227 9(4 6)″
| rowspan="2" align=left | 227,90(460)<ref name="Y"/>
| rowspan="2" | 14.311(289)
| rowspan="2" | 14,312(289)
| rowspan="2" |
|-
|-
| Wolf&nbsp;424&nbsp;B
| style="background-color: #CCC;" | Gl 473 B (FL Virginis)
| 51
<!--- No other name --->| style="background-color: #F99;" | M7Ve
| style="background: {{estrela-cor|M}};" | M7Ve
| 13.17
| 13,17<ref name=RECONS />
| 14.96
| 14,96<ref name=RECONS />
| -
|-
|-
| 37
| style="background-color: #CCC;" | 34
| colspan="2" style="background-color: #CCC;" | [[TZ Arietis]] (GJ 83.1, Luyten 1159-16)
| colspan="2" | [[TZ Arietis|TZ&nbsp;Arietis]] (Gliese 83.1, Luyten&nbsp;1159-16)
| 53
| style="background-color: #F99;" | M4.5V
| style="background: {{estrela-cor|M}};" | M4.5V<ref name=RECONS />
| 12.27
| 12,27<ref name=RECONS />
| 14.03
| 14,03<ref name=RECONS />
| -
| {{RA|02|00|13}}
| {{RA|02|00|13,2}}
| {{DEC|+13|03|08}}
| {{DEC|+13|03|08}}
| align=left | 224,80(290)<ref name="Y"/>
| 0.224 8(2 9)″
| 14.509(188)
| 14,509(187)
|
|-
|-
| 38
| style="background-color: #CCC;" | 35
| colspan="2" style="background-color: #CCC;" | [[Gl 687]] (LHS 450, BD+68°946)
| colspan="2" | [[Gliese 687]] (LHS&nbsp;450, BD+68°946)
| 54
| style="background-color: #F99;" | M3.0V
| style="background: {{estrela-cor|M}};" | M3.0V<ref name=RECONS />
| 9.17
| 9,17<ref name=RECONS />
| 10.89
| 10,89<ref name=RECONS />
| -
| {{RA|17|36|26}}
| {{RA|17|36|25,9}}
| {{DEC|+68|20|21}}
| {{DEC|+68|20|21}}
| align=left | 220,49(082)<ref name="Y"/><ref name="H"/>
| 0.220 5(0 9)″
| 14.792(55)
| 14,793(55)
|
|-
|-
| 39
| style="background-color: #CCC;" | 36
| colspan="2" style="background-color: #CCC;" | [[LHS 292]] (LP 731-58)
| colspan="2" | [[LHS 292|LHS&nbsp;292]] (LP&nbsp;731-58)
| 55
| style="background-color: #F99;" | M6.5V
| style="background: {{estrela-cor|M}};" | M6.5V<ref name=RECONS />
| 15.60
| 15,60<ref name=RECONS />
| 17.32
| 17,32<ref name=RECONS />
| -
| {{RA|10|48|13}}
| {{RA|10|48|12,6}}
| {{DEC|−11|20|02}}
| {{DEC|−11|20|14}}
| align=left | 220,30(360)<ref name="Y"/>
| 0.220 3(3 6)″
| 14.805(243)
| 14,805(242)
|
|-
|-
| 40
| style="background-color: #CCC;" | 37
| colspan="2" style="background-color: #CCC;" | [[Gl 674]] (LHS 449)
| colspan="2" | [[Gliese 674]] (LHS&nbsp;449)
| 56
| style="background-color: #F99;" | M3.0V
| style="background: {{estrela-cor|M}};" | M3.0V<ref name=RECONS />
| 9.38
| 9,38<ref name=RECONS />
| 11.09
| 11,09<ref name=RECONS />
| -
| {{RA|17|28|40}}
| {{RA|17|28|39,9}}
| {{DEC|−46|53|43}}
| {{DEC|−46|53|43}}
| align=left | 220,25(159)<ref name="Y"/><ref name="H"/>
| 0.220 3(1 6)″
| 14.808(107)
| 14,809(107)
| tem um planeta<ref>http://exoplanet.eu/star.php?st=GJ+674</ref>
|-
|-
| rowspan="3" style="background-color: #CCC;" | 38
| rowspan="3" | 41
| rowspan="3" style="background-color: #CCC;" | [[GJ 1245]] (V1581 Cygni)
| rowspan="3" | [[GJ 1245]]
| GJ&nbsp;1245&nbsp;A
| style="background-color: #CCC;" | GJ 1245 A
| 57
| style="background-color: #F99;" | M5.5V
| style="background: {{estrela-cor|M}};" | M5.5V<ref name=RECONS />
| 13.46
| 13,46<ref name=RECONS />
| 15.17
| 15,17<ref name=RECONS />
| -
| {{RA|19|53|54}}
| {{RA|19|53|54,2}}
| {{DEC|−44|24|55}}
| {{DEC|+44|24|55}}
| rowspan="3" | 0.220 2(1 0)″
| rowspan="3" align=left | 220,20(100)<ref name="Y"/>
| rowspan="3" | 14.812(68)
| rowspan="3" | 14,812(67)
| rowspan="3" |
|-
|-
| GJ&nbsp;1245&nbsp;B
| style="background-color: #CCC;" | GJ 1245 B
| 57
| style="background-color: #F99;" | M6.0V
| style="background: {{estrela-cor|M}};" | M6.0V<ref name=RECONS />
| 14.01
| 14,01<ref name=RECONS />
| 15.72
| 15,72<ref name=RECONS />
| -
| {{RA|19|53|55}}
| {{RA|19|53|55,2}}
| {{DEC|−44|24|56}}
| {{DEC|+44|24|56}}
|-
|-
| GJ&nbsp;1245&nbsp;C
| style="background-color: #CCC;" | GJ 1245 C
| 57
| style="background-color: #F99;" | M?
| style="background: {{estrela-cor|M}};" | M5.5
| 16.75
| 16,75<ref name=RECONS />
| 18.46
| 18,46<ref name=RECONS />
| -
| {{RA|19|53|54}}
| {{RA|19|53|54,2}}
| {{DEC|−44|24|55}}
| {{DEC|+44|24|55}}
|-
|-
| 42
| style="background-color: #CCC;" | 39
| colspan="2" style="background-color: #CCC;" | [[GJ 440]] (WD 1142-645)
| colspan="2" | [[Gliese 440]] (WD&nbsp;1142-645)
| 60
| bgcolor="F0F0F0" | DQ6
| style="background: #F0F0F0" | [[Anã branca|DQ6]]<ref name=RECONS />
| 11.50
| 11,50<ref name=RECONS />
| 13.18
| 13,18<ref name=RECONS />
| -
| {{RA|11|45|43}}
| {{RA|11|45|42,9}}
| {{DEC|−64|50|29}}
| {{DEC|−64|50|29}}
|align=left | 216,57(201)<ref name="Y"/><ref name="H"/>
| 0.216 6(2 1)″
| 15.060(140)
| 15,060(140)
|
|-
|-
| 43
| style="background-color: #CCC;" | 40
| colspan="2" style="background-color: #CCC;" | [[GJ 1002]]
| colspan="2" | [[GJ 1002]]
| 61
| style="background-color: #F99;" | M5.5V
| style="background: {{estrela-cor|M}};" | M5.5V<ref name=RECONS />
| 13.76
| 13,76<ref name=RECONS />
| 15.40
| 15,40<ref name=RECONS />
| -
| {{RA|00|06|44}}
| {{RA|00|06|43,8}}
| {{DEC|−07|32|22}}
| {{DEC|−07|32|22}}
| align=left | 213,00(360)<ref name="Y"/>
| 0.213 0(3 6)″
| 15.313(259)
| 15,313(259)
|
|-
|-
| 44
| style="background-color: #CCC;" | 41
| colspan="2" style="background-color: #CCC;" | [[Ross 780]] (GJ 876)
| colspan="2" | [[Gliese 876]] (Ross&nbsp;780)
| 62
| style="background-color: #F99;" | M3.5V
| style="background: {{estrela-cor|M}};" | M3.5V<ref name=RECONS />
| 10.17
| 10,17<ref name=RECONS />
| 11.81
| 11,81<ref name=RECONS />
| -
| {{RA|22|53|17}}
| {{RA|22|53|16,7}}
| {{DEC|−14|15|49}}
| {{DEC|−14|15|49}}
| align=left | 212,59(196)<ref name="Y"/><ref name="H"/>
| 0.212 6(2 0)″
| 15.342(142)
| 15,342(141)
| tem quatro planetas<ref>{{cite journal| last1=Rivera | first1=Eugenio J.| last2=Laughlin | first2=Gregory| last3=Butler | first3=R. Paul| last4=Vogt | first4=Steven S.| last5=Haghighipour | first5=Nader| last6=Meschiari | first6=Stefano| display-authors=1| title=The Lick-Carnegie Exoplanet Survey: A Uranus-mass Fourth Planet for GJ 876 in an Extrasolar Laplace Configuration| journal=The Astrophysical Journal| volume=719| issue=1| pages=890–899| date=julho de 2010| doi=10.1088/0004-637X/719/1/890| bibcode=2010ApJ...719..890R | arxiv=1006.4244}}</ref>
|-
|-
| 45
| style="background-color: #CCC;" | 42
| colspan="2" style="background-color: #CCC;" | [[LHS 288]] (Luyten 143-23)
| colspan="2" | [[LHS 288|LHS&nbsp;288]] (Luyten&nbsp;143-23)
| 63
| style="background-color: #F99;" | M5.5V
| style="background: {{estrela-cor|M}};" | M5.5V<ref name=RECONS />
| 13.92
| 13,90<ref name=RECONS />
| 15.66
| 15,51<ref name=RECONS />
| -
| {{RA|10|44|32}}
| {{RA|10|44|21,2}}
| {{DEC|−61|11|38}}
| {{DEC|−61|12|36}}
| align=left | 208,95(273)<ref name="recent"/>
| style="color: red;" | 0.209 0(2 8)″
| style="color: red;" | 15.609(204)
| 15,610(204)
| <ref name=henry2006 />
|-
|-
| 46
| rowspan="2" style="background-color: #CCC;" | 43
| rowspan="2" style="background-color: #CCC;" | [[GJ 412]]
| style="background: #C67B30" colspan="2" | [[WISE 1405+5534]]
| 64
| style="background-color: #CCC;" | GJ 412 A
| style="background-color: #F99;" | M1.0V
| style="background: {{estrela-cor|Y}};" | [[Anã marrom|Y0p]]
| 20,09 J<ref name="Kirkpatrick2012v1"/>
| 8.77
| 10.34
|
|| {{RA|14|05}}
| -
| {{RA|11|05|29}}
|| {{DEC|+55|34}}
| 207 <ref name="Kirkpatrick2012v1" />
| 15,757<ref name="Kirkpatrick2012v1">{{cite arXiv |last=Kirkpatrick |first=J. Davy |coauthors=Gelino; Cushing; Mace; Griffith; Skrutskie; Marsh; Wright; Eisenhardt; McLean; Mainzer; Burgasser; Tinney; Parker; Salter |title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf mass Function |year=2012 |eprint=1205.2122 |version=v1 |class=astro-ph.SR}}</ref>
|
|-
| rowspan="2" | 47
| rowspan="2" | [[Gliese 412]]
| Gliese 412&nbsp;A
| 65
| style="background: {{estrela-cor|M}};" | M1.0V<ref name=RECONS />
| 8,77<ref name=RECONS />
| 10,34<ref name=RECONS />
| {{RA|11|05|28,6}}
| {{DEC|+43|31|36}}
| {{DEC|+43|31|36}}
| rowspan="2" | 0.206 0(1 1)″
| rowspan="2" align=left | 206,02(108)<ref name="Y"/><ref name="H"/>
| rowspan="2" | 15.831(83)
| rowspan="2" | 15,832(83)
| rowspan="2" |
|-
|-
| style="background-color: #CCC;" | WX Ursae Majoris
| Gliese 412&nbsp;B (WX&nbsp;Ursae&nbsp;Majoris)
| 65
| style="background-color: #F99;" | M5.5V
| style="background: {{estrela-cor|M}};" | M5.5V<ref name=RECONS />
| 14.48
| 14,48<ref name=RECONS />
| 16.05
| 16,05<ref name=RECONS />
| -
| {{RA|11|05|30}}
| {{RA|11|05|30,4}}
| {{DEC|+43|31|18}}
| {{DEC|+43|31|18}}
|-
|-
| 48
| style="background-color: #CCC;" | 44
| colspan="2" style="background-color: #CCC;" | [[Groombridge 1618]] (GJ 380)
| colspan="2" | [[Groombridge 1618|Groombridge&nbsp;1618]] (Gliese 380)
| 67
| style="background-color: #FC9;" | K7.0V
| style="background: {{estrela-cor|K}};" | [[anã laranja|K7.0V]]<ref name=RECONS />
| 6.59
| 6,59<ref name=RECONS />
| 8.16
| 8,16<ref name=RECONS />
| -
| {{RA|10|11|22}}
| {{RA|10|11|22,1}}
| {{DEC|+49|27|15}}
| {{DEC|+49|27|15}}
|align=left | 205,81(067)<ref name="Y"/><ref name="H"/>
| 0.205 8(0 7)″
| 15.847(52)
| 15,848(52)
|
|-
|-
| 49
| style="background-color: #CCC;" | 45
| colspan="2" style="background-color: #CCC;" | [[GJ 388]]
| colspan="2" | [[AD Leonis|AD&nbsp;Leonis]]
| 68
| style="background-color: #F99;" | M3.0V
| style="background: {{estrela-cor|M}};" | M3.0V<ref name=RECONS />
| 9.32
| 9,32<ref name=RECONS />
| 10.87
| 10,87<ref name=RECONS />
| -
| {{RA|10|19|36}}
| {{RA|10|19|36,4}}
| {{DEC|+19|52|10}}
| {{DEC|+19|52|10}}
| align=left | 204,60(280)<ref name="Y"/>
| 0.204 6(2 8)″
| 15.941(219)
| 15,942(218)
|
|-
|-
| 50
| style="background-color: #CCC;" | 46
| colspan="2" style="background-color: #CCC;" | [[GJ 832]]
| style="background: #C67B30" colspan="2" | [[DENIS J081730.0-615520]]
| 69
| style="background-color: #F99;" | M3.0V
| style="background: {{estrela-cor|T}};" | [[Anã marrom|T6]]
| 8.66
| 10.20
|
| -
|
| {{RA|21|33|34}}
|| {{RA|08|17}}
|| {{DEC|-61|55}}
| 203 <ref name="Kirkpatrick2012v1" />
| 16,067<ref name="Kirkpatrick2012v1">{{cite arXiv |last=Kirkpatrick |first=J. Davy |coauthors=Gelino; Cushing; Mace; Griffith; Skrutskie; Marsh; Wright; Eisenhardt; McLean; Mainzer; Burgasser; Tinney; Parker; Salter |title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf mass Function |year=2012 |eprint=1205.2122 |version=v1 |class=astro-ph.SR}}</ref>
|
|-
| 51
| colspan="2" | [[Gliese 832]]
| 70
| style="background: {{estrela-cor|M}};" | M3.0V<ref name=RECONS />
| 8,66<ref name=RECONS />
| 10,20<ref name=RECONS />
| {{RA|21|33|34,0}}
| {{DEC|−49|00|32}}
| {{DEC|−49|00|32}}
| align=left | 202,78(132)<ref name="Y"/><ref name="H"/>
| 0.202 8(1 4)″
| 16.084(105)
| 16,085(105)
| tem um planeta<ref>{{cite journal | author=Bailey, Jeremy ''et al.'' | title=A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832 | doi=10.1088/0004-637X/690/1/743 | bibcode=2009ApJ...690..743B | journal=The Astrophysical Journal | volume=690 | issue=1 | pages=743&ndash;747 | year=2008 | accessdate=02/09/2008 | arxiv=0809.0172 }}</ref>
|-
|-
| 52
| style="background-color: #CCC;" | 47
| colspan="2" style="background-color: #CCC;" | [[LP 944-020]]
| style="background: #C67B30" colspan="2" | [[LP 944-020|LP&nbsp;944-020]]
| 71
| style="background-color: #F99;" | M9.0V
| style="background: {{estrela-cor|M}};" | M9.0V<ref name=RECONS />
| 18.50
| 18,50<ref name=RECONS />
| 20.02
| 20,02<ref name=RECONS />
| -
| {{RA|03|39|35}}
| {{RA|03|39|35,2}}
| {{DEC|−35|25|41}}
| {{DEC|−35|25|41}}
| align=left | 201,40(420)<ref name="T">[http://cdsads.u-strasbg.fr/abs/1996MNRAS.281..644T CCD astrometry of southern very low-mass stars], C. G. Tinney, ''Monthly Notices of the Royal Astronomical Society'' '''281''', #2 (julho de 1996), pp. 644&ndash;658.</ref>
| 0.201 4(4 2)″
| 16.194(338)
| 16,195(338)
|
|-
|-
| 53
| style="background-color: #CCC;" | 48
| colspan="2" style="background-color: #CCC;" | [[DEN 0255-4700]]
| style="background: #C67B30" colspan="2" | [[DEN 0255-4700|DEN&nbsp;0255-4700]]
| 72
| style="background-color: #F99;" | L7.5V
| style="background: {{estrela-cor|L}};" | [[Anã marrom|L7.5V]]<ref name=RECONS />
| 22.92
| 22,92<ref name=RECONS />
| 24.44
| 24,44<ref name=RECONS />
| -
| {{RA|02|55|3.7}}
| {{RA|02|55|03,7}}
| {{DEC|−47|00|52}}
| {{DEC|−47|00|52}}
| align=left | 201,37(389)<ref name="recent"/>
| 0.201 4(3 9)″
| 16.197(314)
| 16,197(313)
| <ref name=costa2005 />
|-
|- class="unsortable"
| style="background-color: #CCC;" | 49
! rowspan="2" |#
| colspan="2" style="background-color: #CCC;" | [[GJ 682|GJ&nbsp;682]]
!<small>[[sistema estelar|Sistema]]</small>
| style="background-color: #F99;" | M4.5V
!<small>[[Estrela]]</small>
| 10.95
!<small>Star #</small>
| 12.45
! rowspan="2" |<small>[[Classificação estelar]]</small>
| -
! rowspan="2" |<small>[[Magnitude aparente]] ({{nowrap|m<sub>[[Sistema fotométrico UBV|V]]</sub> ou m<sub>[[banda J|J]]</sub>}})</small>
| {{RA|17|37|04}}
! rowspan="2" |<small>[[Magnitude absoluta]] ({{nowrap|M<sub>[[Sistema fotométrico UBV|V]]</sub> ou M<sub>[[banda J|J]]</sub>}})</small>
| {{DEC|−44|19|09}}
!<small>[[Ascensão reta]]<ref name=RECONS /></small>
| 0.199 7(2 3)″
!<small>[[Declinação]]<ref name=RECONS /></small>
| 16.336(189)
! rowspan="2" |<small>[[Paralaxe]]<ref name="RECONS"/><br>[[segundo de arco|mas]][[margem de erro|(±err)]]</small>
! rowspan="2" |<small>Distância<ref name=distfn /><br>[[ano-luz|anos-luz]][[margem de erro|(±err)]]</small>
! rowspan="2" |<small> Notas adicionais</small>
|-class="unsortable"
! colspan="3" |<small>Designação</small>
! style="background: #FFC" colspan="2" |<small>[[Época (astronomia)|Época]] J2000.0</small>
|}
|}


== Mapa ==
== Mapa ==
O seguinte mapa mostra todos os sistemas estelares a até 14 anos-luz do Sol, exceto duas anãs marrons descobertas após 2009<!---([[UGPS J072227.51-054031.2|UGPS 0722-05]], WISE ... --->. Estrelas duplas e triplas são mostradas "estacadas" verticalmente, sendo que a posição verdadeira é a da estrela mais próxima do plano central. A cor corresponde ao tipo espectral.
[[Ficheiro:Nearby Stars (14ly Radius).svg|centre]]
[[Ficheiro:Nearby Stars (14ly Radius).svg|centre]]

==Futuro e passado==
[[File:Near-stars-past-future-en.svg|right|thumb|350px|Distâncias de algumas estrelas próximas de 20&nbsp;000 anos atrás até 80&nbsp;000 anos no futuro.]]
[[Ross 248]], atualmente a uma distância de 10,3 anos-luz, tem uma [[velocidade radial]] de −81&nbsp;km/s. Em cerca de 31&nbsp;000 anos ela pode ser a estrela mais próxima do Sol por vários milênios, com uma distância mínima de 0,927 parsecs (3,02 anos-luz) em 36&nbsp;000 anos.<ref name=Matthews1994/> [[Gliese 445]], atualmente a 17,6 anos-luz, tem uma velocidade radial de −119&nbsp;km/s. Em cerca de 40&nbsp;000 anos ela vai ser a estrela mais próxima por um período de vários milhares de anos.<ref name=Matthews1994>[http://adsabs.harvard.edu/abs/1994QJRAS..35....1M The Close Approach of Stars in the Solar Neighborhood]</ref>
{{-}}

Estrelas conhecidas que passaram ou vão passar a até 5,1 anos-luz do Sol em ±2 milhões de anos:<ref name="Bobylev:arXiv1003.2160">Table 3, {{cite journal |last=Bobylev |first=Vadim V. |authorlink= |year=2010 |month=March |title=Searching for Stars Closely Encountering with the Solar System |journal=Astronomy Letters |volume=36 |issue=3 |pages=220–226 |doi=10.1134/S1063773710030060 |arxiv=1003.2160 |bibcode=2010AstL...36..220B}} </ref>

{| border="1" class="wikitable sortable" style="width:95%; text-align:center;"
|-----
! Estrela<br/>
! [[catálogo Hipparcos|HIP#]]<br/>
! Distância mínima em [[parsec]]s<br/>
! Distância mínima em [[ano-luz|anos-luz]]<br />
! Data de aproximação em milhares de anos<br/>
! Distância atual em parsecs<br/>
! Distância atual em anos-luz<br/>
! Classificação estelar<br/>
! Massa em [[massa solar|M<sub>☉</sub>]]<br/>
! [[Magnitude aparente]] atual<br/>
! [[Constelação]]<br/>
! [[Ascensão reta]]<br/>
! [[Declinação]]<br/>
|-----
| [[Gliese 710]]
| 89825
| 0,311
| 1,01
| 1447
| 19,3
| 62,9
| K7V
| 0,4–0,6
| 9,6
| [[Serpens]]
| {{RA|18|19|50,843}}
| {{DEC|−01|56|18,98}}
|-----
| [[Proxima Centauri]]
| 70890
| 0,890
| 2,90
| 27,4
| 1,29
| 4,24
| M5Ve
| 0,15
| 11,05
| [[Centaurus]]
| {{RA|14|29|42,949}}
| {{DEC|−62|40|46,14}}
|-----
| [[Alpha Centauri]] A
| 71683
| 0,910
| 2,97
| 28,4
| 1,338
| 4,36
| G2V
| 1,100<ref name=eso0307>[http://www.eso.org/public/news/eso0307/ A&nbsp;Family Portrait of the Alpha Centauri System], eso307, 15 de março de 2003, [[European Southern Observatory]]. Acessado em 24 de janeiro de 2011.</ref>
| −0,01
| [[Centaurus]]
| {{RA|14|39|36,495}}
| {{DEC|−60|50|02,31}}
|-----
| [[Alpha Centauri]] B
| 71681
| 0,910
| 2,97
| 28,4
| 1,338
| 4,36
| K1V
| 0,907<ref name=eso0307 />
| 1,33
| [[Centaurus]]
| {{RA|14|39|35,080}}
| {{DEC|−60|50|13,76}}
|-----
| [[AC+79 3888]]
| 57544
| 1,059
| 3,45
| 46,0
| 5,39
| 17,6
| M4
| 0,15?
| 10,8
| [[Camelopardalis]]
| {{RA|11|47|41,377}}
| {{DEC|+78|41|28,18}}
|-----
| [[Estrela de Barnard]]
| 87937
| 1,148
| 3,74
| 9,8
| 1,834
| 5,98
| sdM4
| 0,144
| 9,54
| [[Ophiuchus]]
| {{RA|17|57|48,498}}
| {{DEC|+04|41|36,25}}
|-----
| [[Zeta Leporis]]
| 27288
| 1,275
| 4,16
| −861
| 21,5
| 70,2
| A2Vann
| 2,0
| 3,55
| [[Lepus]]
| {{RA|05|46|57,341}}
| {{DEC|−14|49|19,02}}
|-----
| [[Lalande 21185]]
| 54035
| 1,426
| 4,65
| 20,5
| 2,55
| 8,32
| M2V
| 0.39
| 7.52
| [[Ursa Major]]
| {{RA|11|03|20,194}}
| {{DEC|+35|58|11,55}}
|-----
| [[Gliese 208]]
| 26335
| 1,537
| 5,01
| −500
| 11,38
| 37,1
| K7
| 0,47
| 8,9
| [[Orion (constelação)|Orion]]
| {{RA|05|36|30,991}}
| {{DEC|+11|19|40,32}}
|}

==Ver também==

* [[Viagem interestelar]]
* [[Anexo:Lista das estrelas mais brilhantes|Lista das estrelas mais brilhantes]]
* [[Anexo:Lista das estrelas brilhantes mais próximas|Lista das estrelas brilhantes mais próximas]]
* [[Anexo:Listas de estrelas|Listas de estrelas]]

{{Referências|col=2}}


{{Localização da Terra no espaço}}
{{Localização da Terra no espaço}}
{{Estrela}}


[[Categoria:Constelação de Draco]]
[[Categoria:Constelação de Draco]]

Revisão das 01h49min de 27 de julho de 2012

Representação artística de uma estrela anã vermelha, o tipo mais comum de estrela na vizinhança do Sol, e no universo. Apesar do nome, a temperatura superficial desse tipo de estrela daria a ela um tom alaranjado quando vista de perto.

Esta lista de estrelas próximas contém todas as estrelas e anãs marrons conhecidas a uma distância de até 5 parsecs (16,3 anos-luz) do Sistema Solar, ordenadas por distância crescente. Além do Sistema Solar, há outros 53 sistemas estelares conhecidos atualmente a até essa distância. Esses sistemas contêm um total de 60 estrelas que fundem hidrogênio e 12 anãs marrons. Apesar de estarem relativamente próximos da Terra, apenas nove desses objetos têm uma magnitude aparente menor que 6,5, o que significa que somente 13% deles podem ser vistos a olho nu.[1] Além do Sol, há apenas três estrela de primeira magnitude: Alpha Centauri, Sirius, e Procyon. Todos esses objetos estão localizados na Bolha Local, uma região no Braço de Órion da Via Láctea.

Lista

Estrelas visíveis a olho nu têm a magnitude aparente destacada em azul claro. Os tipos espectrais das estrelas e anãs marrons são mostrados com sua cor correspondente (essas cores são derivadas do nome convencional das classes espectrais e não representam a cor observada da estrela). Muitas anãs marrons não estão listadas por magnitude visível mas sim por magnitude na banda J. Algumas paralaxes e distância são medições preliminares.[2]

# Designação Classificação estelar Magnitude aparente (mV ou mJ) Magnitude absoluta (MV ou MJ) Época J2000.0 Paralaxe[2]
mas(±err) 		Distância[3]
anos-luz (±err) 		Notas adicionais
Sistema Estrela Estrela # Ascensão reta[2] Declinação[2]
Sistema Solar Sol G2V[2] −26,74[2] 4,85[2] — — 0 tem oito planetas
1 Alpha Centauri
(Rigil Kentaurus) 		Proxima Centauri (V645 Centauri) 1 M5.5Ve 11,09[2] 15,53[2] 14h 29m 43,0s −62° 40′ 46″ 768,87(029)[4][5] 4,2421(16) [6]
α Centauri A (HD 128620) 2 G2V[2] 0,01[2] 4,38[2] 14h 39m 36,5s −60° 50′ 02″ 747,23(117)[4][7] 4,3650(68)
α Centauri B (HD 128621) 2 K1V[2] 1,34[2] 5,71[2] 14h 39m 35,1s −60° 50′ 14″
2 Estrela de Barnard (BD+04°3561a) 4 M4.0Ve 9,53[2] 13,22[2] 17h 57m 48,5s +04° 41′ 36″ 546,98(1 00)[4][5] 5,9630(109)
3 Wolf 359 (CN Leonis) 5 M6.0V[2] 13,44[2] 16,55[2] 10h 56m 29,2s +07° 00′ 53″ 419,10(210)[4] 7,7825(390)
4 Lalande 21185 (BD+36°2147) 6 M2.0V[2] 7,47[2] 10,44[2] 11h 03m 20,2s +35° 58′ 12″ 393,42(070)[4][5] 8,2905(148)
5 Sirius
(α Canis Majoris) 		Sirius A 7 A1V[2] −1,46[2] 1,42[2] 06h 45m 08,9s −16° 42′ 58″ 380,02(128)[4][5] 8,5828(289)
Sirius B 7 DA2[2] 8,44[2] 11,34[2]
6 Luyten 726-8 Luyten 726-8 A (BL Ceti) 9 M5.5Ve 12,54[2] 15,40[2] 01h 39m 01,3s −17° 57′ 01″ 373,70(270)[4] 8,7280(631)
Luyten 726-8 B (UV Ceti) 10 M6.0Ve 12,99[2] 15,85[2]
7 Ross 154 (V1216 Sagittarii) 11 M3.5Ve 10,43[2] 13,07[2] 18h 49m 49,4s −23° 50′ 10″ 336,90(178)[4][5] 9,6813(512)
8 Ross 248 (HH Andromedae) 12 M5.5Ve 12,29[2] 14,79[2] 23h 41m 54,7s +44° 10′ 30″ 316,00(110)[4] 10,322(36)
9 Epsilon Eridani (BD−09°697) 13 K2V[2] 3,73[2] 6,19[2] 03h 32m 55,8s −09° 27′ 30″ 309,99(079)[4][5] 10,522(27) acredita-se que tem dois planetas[8]
10 Lacaille 9352 (CD−36°15693) 14 M1.5Ve 7,34[2] 9,75[2] 23h 05m 52,0s −35° 51′ 11″ 303,64(087)[4][5] 10,742(31)
11 Ross 128 (FI Virginis) 15 M4.0Vn 11,13[2] 13,51[2] 11h 47m 44,4s +00° 48′ 16″ 298,72(135)[4][5] 10,919(49)
12 EZ Aquarii
(Gliese 866, Luyten 789-6) 		EZ Aquarii A 16 M5.0Ve 13,33[2] 15,64[2] 22h 38m 33,4s −15° 18′ 07″ 289,50(440)[4] 11,266(171)
EZ Aquarii B 16 M? 13,27[2] 15,58[2]
EZ Aquarii C 16 M? 14,03[2] 16,34[2]
13 Procyon
(α Canis Minoris) 		Procyon A 19 F5V-IV[2] 0,38[2] 2,66[2] 07h 39m 18,1s +05° 13′ 30″ 286,05(081)[4][5] 11,402(32)
Procyon B 19 DA[2] 10,70[2] 12,98[2]
14 61 Cygni 61 Cygni A (BD+38°4343) 21 K5.0V[2] 5,21[2] 7,49[2] 21h 06m 53,9s +38° 44′ 58″ 286,04(056)[4][5] 11,403(22) primeira estrela (além do Sol) a ter sua distância medida[9]
61 Cygni B (BD+38°4344) 21 K7.0V[2] 6,03[2] 8,31[2] 21h 06m 55,3s +38° 44′ 31″
15 Struve 2398
(Gliese 725, BD+59°1915) 		Struve 2398 A (HD 173739) 23 M3.0V[2] 8,90[2] 11,16[2] 18h 42m 46,7s +59° 37′ 49″ 283,00(169)[4][5] 11,525(69)
Struve 2398 B (HD 173740) 23 M3.5V[2] 9,69[2] 11,95[2] 18h 42m 46,9s +59° 37′ 37″
16 Groombridge 34
(Gliese 15) 		Groombridge 34 A (GX Andromedae) 25 M1.5V[2] 8,08[2] 10,32[2] 0h 18m 22,9s +44° 01′ 23″ 280,59(095)[4][5] 11,624(39)
Groombridge 34 B (GQ Andromedae) 25 M3.5V[2] 11,06[2] 13,30[2]
17 Epsilon Indi
(CPD−57°10015) 		Epsilon Indi A 27 K5Ve[2] 4,69[2] 6,89[2] 22h 03m 21,7s −56° 47′ 10″ 275,84(069)[4][5] 11,824(30)
Epsilon Indi Ba 27 T1.0V 12,3 J[10] 22h 04m 10,5s −56° 46′ 58″
Epsilon Indi Bb 27 T6.0V 13,2 J[10]
18 DX Cancri (G 51-15) 30 M6.5Ve 14,78[2] 16,98[2] 08h 29m 49,5s +26° 46′ 37″ 275,80(300)[4] 11,826(129)
19 Tau Ceti (BD−16°295) 31 G8Vp[2] 3,49[2] 5,68[2] 01h 44m 04,1s −15° 56′ 15″ 274,39(076)[4][5] 11,887(33)
20 GJ 1061 (LHS 1565) 32 M5.5V[2] 13,09[2] 15,26[2] 03h 35m 59,7s −44° 30′ 45″ 272,01(130)[11] 11,991(57) [12][13]
21 YZ Ceti (LHS 138) 33 M4.5V[2] 12,02[2] 14,17[2] 01h 12m 30,6s −16° 59′ 56″ 268,84(295)[4][5] 12,132(133)
22 Estrela de Luyten (BD+05°1668) 34 M3.5Vn 9,86[2] 11,97[2] 07h 27m 24,5s +05° 13′ 33″ 263,76(125)[4][5] 12,366(59)
23 Estrela de Teegarden (SO025300.5+165258) 35 M6.5V 15,14[2] 17,22[2] 02h 53m 00,9s +16° 52′ 53″ 260,63(269)[11] 12,514(129) [13]
24 SCR 1845-6357 SCR 1845-6357 A 36 M8.5V[2] 17,39 19,41 18h 45m 05,3s −63° 57′ 48″ 259,45(111)[11] 12,571(54) [13]
SCR 1845-6357 B 36 T6[14] 13,3 J[10] 18h 45m 02,6s −63° 57′ 52″
25 Estrela de Kapteyn (CD−45°1841) 38 M1.5V[2] 8,84[2] 10,87[2] 05h 11m 40,6s −45° 01′ 06″ 255,27(086)[4][5] 12,777(43)
26 Lacaille 8760 (AX Microscopii) 39 M0.0V[2] 6,67[2] 8,69[2] 21h 17m 15,3s −38° 52′ 03″ 253,43(112)[4][5] 12,870(57)
27 Kruger 60
(BD+56°2783) 		Kruger 60 A 40 M3.0V[2] 9,79[2] 11,76[2] 22h 27m 59,5s +57° 41′ 45″ 248,06(139)[4][7] 13,149(74)
Kruger 60 B (DO Cephei) 40 M4.0V[2] 11,41[2] 13,38[2]
28 DEN 1048-3956 42 M8.5V[2] 17,39[2] 19,37[2] 10h 48m 14,7s −39° 56′ 06″ 247,71(155)[11] 13,167(82) [15][16]
29 UGPS 0722-05 43 T9[2] 16,52 J[17] 07h 22m 27,3s –05° 40′ 30″ 246 13,259 [18]
30 Ross 614
(V577 Monocerotis, Gliese 234) 		Ross 614A (LHS 1849) 44 M4.5V[2] 11,15[2] 13,09[2] 06h 29m 23,4s −02° 48′ 50″ 244,34(201)[4][7] 13,349(110)
Ross 614B (LHS 1850) 44 M5.5V 14,23[2] 16,17[2]
31 WISE 1541-2250 46 Y0.5 20,74 J[19] 15h 41m 51,57s −22° 50′ 25″ 238 [19] 13,704[19]
32 WISE 0350-5658 47 Y1 >22,8 J[19] 03h 50m −56° 58′ 238 [19] 13,704[19]
33 Wolf 1061 (Gliese 628, BD−12°4523) 48 M3.0V[2] 10,07[2] 11,93[2] 16h 30m 18,1s −12° 39′ 45″ 236,01(167)[4][5] 13,820(98)
34 Estrela de van Maanen (Gliese 35, LHS 7) 49 DZ7[2] 12,38[2] 14,21[2] 00h 49m 09,9s +05° 23′ 19″ 231,88(179)[4][5] 14,066(109)
35 Gliese 1 (CD−37°15492) 50 M3.0V[2] 8,55[2] 10,35[2] 00h 05m 24,4s −37° 21′ 27″ 229,20(107)[4][5] 14,231(66)
36 Wolf 424
(FL Virginis, LHS 333, Gliese 473) 		Wolf 424 A 51 M5.5Ve 13,18[2] 14,97[2] 12h 33m 17,2s +09° 01′ 15″ 227,90(460)[4] 14,312(289)
Wolf 424 B 51 M7Ve 13,17[2] 14,96[2]
37 TZ Arietis (Gliese 83.1, Luyten 1159-16) 53 M4.5V[2] 12,27[2] 14,03[2] 02h 00m 13,2s +13° 03′ 08″ 224,80(290)[4] 14,509(187)
38 Gliese 687 (LHS 450, BD+68°946) 54 M3.0V[2] 9,17[2] 10,89[2] 17h 36m 25,9s +68° 20′ 21″ 220,49(082)[4][5] 14,793(55)
39 LHS 292 (LP 731-58) 55 M6.5V[2] 15,60[2] 17,32[2] 10h 48m 12,6s −11° 20′ 14″ 220,30(360)[4] 14,805(242)
40 Gliese 674 (LHS 449) 56 M3.0V[2] 9,38[2] 11,09[2] 17h 28m 39,9s −46° 53′ 43″ 220,25(159)[4][5] 14,809(107) tem um planeta[20]
41 GJ 1245 GJ 1245 A 57 M5.5V[2] 13,46[2] 15,17[2] 19h 53m 54,2s +44° 24′ 55″ 220,20(100)[4] 14,812(67)
GJ 1245 B 57 M6.0V[2] 14,01[2] 15,72[2] 19h 53m 55,2s +44° 24′ 56″
GJ 1245 C 57 M5.5 16,75[2] 18,46[2] 19h 53m 54,2s +44° 24′ 55″
42 Gliese 440 (WD 1142-645) 60 DQ6[2] 11,50[2] 13,18[2] 11h 45m 42,9s −64° 50′ 29″ 216,57(201)[4][5] 15,060(140)
43 GJ 1002 61 M5.5V[2] 13,76[2] 15,40[2] 00h 06m 43,8s −07° 32′ 22″ 213,00(360)[4] 15,313(259)
44 Gliese 876 (Ross 780) 62 M3.5V[2] 10,17[2] 11,81[2] 22h 53m 16,7s −14° 15′ 49″ 212,59(196)[4][5] 15,342(141) tem quatro planetas[21]
45 LHS 288 (Luyten 143-23) 63 M5.5V[2] 13,90[2] 15,51[2] 10h 44m 21,2s −61° 12′ 36″ 208,95(273)[11] 15,610(204) [13]
46 WISE 1405+5534 64 Y0p 20,09 J[19] 14h 05m +55° 34′ 207 [19] 15,757[19]
47 Gliese 412 Gliese 412 A 65 M1.0V[2] 8,77[2] 10,34[2] 11h 05m 28,6s +43° 31′ 36″ 206,02(108)[4][5] 15,832(83)
Gliese 412 B (WX Ursae Majoris) 65 M5.5V[2] 14,48[2] 16,05[2] 11h 05m 30,4s +43° 31′ 18″
48 Groombridge 1618 (Gliese 380) 67 K7.0V[2] 6,59[2] 8,16[2] 10h 11m 22,1s +49° 27′ 15″ 205,81(067)[4][5] 15,848(52)
49 AD Leonis 68 M3.0V[2] 9,32[2] 10,87[2] 10h 19m 36,4s +19° 52′ 10″ 204,60(280)[4] 15,942(218)
50 DENIS J081730.0-615520 69 T6 08h 17m -61° 55′ 203 [19] 16,067[19]
51 Gliese 832 70 M3.0V[2] 8,66[2] 10,20[2] 21h 33m 34,0s −49° 00′ 32″ 202,78(132)[4][5] 16,085(105) tem um planeta[22]
52 LP 944-020 71 M9.0V[2] 18,50[2] 20,02[2] 03h 39m 35,2s −35° 25′ 41″ 201,40(420)[23] 16,195(338)
53 DEN 0255-4700 72 L7.5V[2] 22,92[2] 24,44[2] 02h 55m 03,7s −47° 00′ 52″ 201,37(389)[11] 16,197(313) [16]
# Sistema Estrela Star # Classificação estelar Magnitude aparente (mV ou mJ) Magnitude absoluta (MV ou MJ) Ascensão reta[2] Declinação[2] Paralaxe[2]
mas(±err) 		Distância[3]
anos-luz(±err) 		Notas adicionais
Designação Época J2000.0

Mapa

O seguinte mapa mostra todos os sistemas estelares a até 14 anos-luz do Sol, exceto duas anãs marrons descobertas após 2009. Estrelas duplas e triplas são mostradas "estacadas" verticalmente, sendo que a posição verdadeira é a da estrela mais próxima do plano central. A cor corresponde ao tipo espectral.

Futuro e passado

Distâncias de algumas estrelas próximas de 20 000 anos atrás até 80 000 anos no futuro.

Ross 248, atualmente a uma distância de 10,3 anos-luz, tem uma velocidade radial de −81 km/s. Em cerca de 31 000 anos ela pode ser a estrela mais próxima do Sol por vários milênios, com uma distância mínima de 0,927 parsecs (3,02 anos-luz) em 36 000 anos.[24] Gliese 445, atualmente a 17,6 anos-luz, tem uma velocidade radial de −119 km/s. Em cerca de 40 000 anos ela vai ser a estrela mais próxima por um período de vários milhares de anos.[24]

Estrelas conhecidas que passaram ou vão passar a até 5,1 anos-luz do Sol em ±2 milhões de anos:[25]

Estrela
 HIP#
 Distância mínima em parsecs
 Distância mínima em anos-luz
 Data de aproximação em milhares de anos
 Distância atual em parsecs
 Distância atual em anos-luz
 Classificação estelar
 Massa em M☉
 Magnitude aparente atual
 Constelação
 Ascensão reta
 Declinação
Gliese 710 89825 0,311 1,01 1447 19,3 62,9 K7V 0,4–0,6 9,6 Serpens 18h 19m 50,843s −01° 56′ 18,98″
Proxima Centauri 70890 0,890 2,90 27,4 1,29 4,24 M5Ve 0,15 11,05 Centaurus 14h 29m 42,949s −62° 40′ 46,14″
Alpha Centauri A 71683 0,910 2,97 28,4 1,338 4,36 G2V 1,100[26] −0,01 Centaurus 14h 39m 36,495s −60° 50′ 02,31″
Alpha Centauri B 71681 0,910 2,97 28,4 1,338 4,36 K1V 0,907[26] 1,33 Centaurus 14h 39m 35,080s −60° 50′ 13,76″
AC+79 3888 57544 1,059 3,45 46,0 5,39 17,6 M4 0,15? 10,8 Camelopardalis 11h 47m 41,377s +78° 41′ 28,18″
Estrela de Barnard 87937 1,148 3,74 9,8 1,834 5,98 sdM4 0,144 9,54 Ophiuchus 17h 57m 48,498s +04° 41′ 36,25″
Zeta Leporis 27288 1,275 4,16 −861 21,5 70,2 A2Vann 2,0 3,55 Lepus 05h 46m 57,341s −14° 49′ 19,02″
Lalande 21185 54035 1,426 4,65 20,5 2,55 8,32 M2V 0.39 7.52 Ursa Major 11h 03m 20,194s +35° 58′ 11,55″
Gliese 208 26335 1,537 5,01 −500 11,38 37,1 K7 0,47 8,9 Orion 05h 36m 30,991s +11° 19′ 40,32″

Ver também

Referências

  1. ↑ Weaver, Harold F. (1947). «The Visibility of Stars Without Optical Aid». Publications of the Astronomical Society of the Pacific. 59 (350): 232–243. Bibcode:1947PASP...59..232W. doi:10.1086/125956 
  2. ↑ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al am an ao ap aq ar as at au av aw ax ay az ba bb bc bd be bf bg bh bi bj bk bl bm bn bo bp bq br bs bt bu bv bw bx by bz ca cb cc cd ce cf cg ch ci cj ck cl cm cn co cp cq cr cs ct cu cv cw cx cy cz da db dc dd de df dg dh di dj dk dl dm dn do dp dq dr ds dt du dv dw dx dy dz ea eb ec ed ee ef eg eh ei ej ek el em en eo ep eq er es et eu ev ew ex ey ez fa fb fc fd fe ff fg fh fi fj fk fl fm fn fo fp fq fr fs ft fu fv fw fx fy fz ga Research Consortium on Nearby Stars, GSU (17 de setembro de 2007). «The One Hundred Nearest Star Systems». RECONS. Consultado em 6 de novembro de 2007 
  3. ↑ a b Calculada a partir do paralaxe.
  4. ↑ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al am an ao ap General Catalogue of Trigonometric Parallaxes.
  5. ↑ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab Catálogo Hipparcos.
  6. ↑ Burgasser et al. 2000
  7. ↑ a b c Visual binary orbits and masses post Hipparcos, Staffan Söderhjelm, Astronomy and Astrophysics 341 (janeiro de 1999), pp. 121–140.
  8. ↑ Janson, M.; et al. (setembro de 2008), «A comprehensive examination of the ε Eridani system. Verification of a 4 micron narrow-band high-contrast imaging approach for planet searches», Astronomy and Astrophysics, 488 (2): 771–780, Bibcode:2008A&A...488..771J, arXiv:0807.0301Acessível livremente, doi:10.1051/0004-6361:200809984 
  9. ↑ Bessel, F. W. (1839). «Bestimmung der Entfernung des 61sten Sterns des Schwans. Von Herrn Geheimen - Rath und Ritter Bessel». Astronomische Nachrichten (em German). 16 (5-6). 65 páginas. Bibcode:1839AN.....16...65B. doi:10.1002/asna.18390160502. (page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist  A parallax of 313.6 mas yields a distance of 10.4 light years
  10. ↑ a b c Chris Gelino, Davy Kirkpatrick, Adam Burgasser. «DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs». caltech.edu. Consultado em 10 de junho de 2012  (main page)
  11. ↑ a b c d e f Systems with their first accurate trigonometric parallaxes measured by RECONS
  12. ↑ The solar neighborhood IV: discovery of the twentieth nearest star, Todd J. Henry, Philip A. Ianna, J. Davy Kirkpatrick, Hartmut Jahreiss, The Astronomical Journal 114, #1 (julho de 1997), pp. 388–395. doi:10.1086/118482
  13. ↑ a b c d The Solar Neighborhood. XVII. Parallax Results from the CTIOPI 0.9 m Program: 20 New Members of the RECONS 10 Parsec Sample, Todd J. Henry, Wei-Chun Jao, John P. Subasavage, Thomas D. Beaulieu, Philip A. Ianna, Edgardo Costa, René A. Méndez, The Astronomical Journal 132, #6 (dezembro de 2006), pp. 2360–2371. doi:10.1086/508233
  14. ↑ The very nearby M/T dwarf binary SCR 1845-6357, Markus Kasper, Beth A. Biller, Adam Burrows, Wolfgang Brandner, Jano Budaj, and Laird M. Close, Astronomy and Astrophysics 471, #2 (agosto de 2007), pp. 655–659. doi:10.1051/0004-6361:20077881
  15. ↑ The Solar Neighborhood. XIII. Parallax Results from the CTIOPI 0.9 Meter Program: Stars with μ >= 1.0" yr-1 (Motion sample), Wei-Chun Jao, Todd J. Henry, John P. Subasavage, Misty A. Brown, Philip A. Ianna, Jennifer L. Bartlett, Edgardo Costa, René A. Méndez, The Astronomical Journal 129, #4 (abril de 2005), pp. 1954–1967. doi:10.1086/428489
  16. ↑ a b The Solar Neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation—First Results from the 1.5 m Telescope Program, Edgardo Costa, René A. Méndez, W.-C. Jao, Todd J. Henry, John P. Subasavage, Misty A. Brown, Philip A. Ianna, and Jennifer Bartlett, The Astronomical Journal 130, #1 (julho de 2005), pp. 337–349. doi:10.1086/430473
  17. ↑ Lucas; Tinney; Ben Burningham; Leggett; Pinfield; Richard Smart; Jones; Federico Marocco; Barber (2010). «The discovery of a very cool, very nearby brown dwarf in the Galactic plane». arXiv:1004.0317v2Acessível livremente [astro-ph.SR] 
  18. ↑ Lucas, Philip W.; Tinney; Burningham; Leggett; Pinfield; Smart; et al. (2010). «Discovery of a very cool brown dwarf amongst the ten nearest stars to the Solar System». arXiv:1004.0317v1Acessível livremente [astro-ph.SR] 
  19. ↑ a b c d e f g h i j k Kirkpatrick, J. Davy; Gelino; Cushing; Mace; Griffith; Skrutskie; Marsh; Wright; Eisenhardt; McLean; Mainzer; Burgasser; Tinney; Parker; Salter (2012). «Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf mass Function». arXiv:1205.2122v1Acessível livremente [astro-ph.SR] 
  20. ↑ http://exoplanet.eu/star.php?st=GJ+674
  21. ↑ Rivera, Eugenio J.; et al. (julho de 2010). «The Lick-Carnegie Exoplanet Survey: A Uranus-mass Fourth Planet for GJ 876 in an Extrasolar Laplace Configuration». The Astrophysical Journal. 719 (1): 890–899. Bibcode:2010ApJ...719..890R. arXiv:1006.4244Acessível livremente. doi:10.1088/0004-637X/719/1/890 
  22. ↑ Bailey, Jeremy; et al. (2008). «A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832». The Astrophysical Journal. 690 (1): 743–747. Bibcode:2009ApJ...690..743B. arXiv:0809.0172Acessível livremente. doi:10.1088/0004-637X/690/1/743 
  23. ↑ CCD astrometry of southern very low-mass stars, C. G. Tinney, Monthly Notices of the Royal Astronomical Society 281, #2 (julho de 1996), pp. 644–658.
  24. ↑ a b The Close Approach of Stars in the Solar Neighborhood
  25. ↑ Table 3, Bobylev, Vadim V. (2010). «Searching for Stars Closely Encountering with the Solar System». Astronomy Letters. 36 (3): 220–226. Bibcode:2010AstL...36..220B. arXiv:1003.2160Acessível livremente. doi:10.1134/S1063773710030060 
  26. ↑ a b A Family Portrait of the Alpha Centauri System, eso307, 15 de março de 2003, European Southern Observatory. Acessado em 24 de janeiro de 2011.
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