卡普坦星：修订间差异

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{{Translating |time=2014-6-10}}
{{Request translation|tfrom=[[:en:Kapteyn's Star]]}}

{{Starbox begin |
{{Starbox begin |
name=卡普坦星}}
name=卡普坦星}}
第10行： 第9行：
caption=紅點是卡普坦星在繪架座的位置。
caption=紅點是卡普坦星在繪架座的位置。
}}
}}
{{Starbox observe |
{{Starbox observe
epoch=J2000 |
| epoch = J2000
constell=[[繪架座]] |
| constell = [[繪架座]]
| ra = {{RA|05|11|40.58112}}<ref name="aaa474_2_653"/>
ra=05h 11m 40.6s |
dec=-45° 01' 06" |
| dec = {{DEC|-45|01|06.2899}}<ref name="aaa474_2_653"/>
appmag_v=8.85 }}
| appmag_v = 8.853<ref name="mnras403_4_1949"/>
}}
{{Starbox character |
{{Starbox character
class=sdM1 V |
| class = sdM1<ref name="mnras403_4_1949"/>
b-v=1.56 |
| b-v = +1.57<ref name="SIMBAD"/>
u-b=1.15 |
| u-b = +1.21<ref name="SIMBAD"/>
variable=''Unknown'' }}
| variable = [[天龍座BY型變星]]<ref name="var"/>
{{Starbox astrometry |
}}
radial_v=+245.5 |
{{Starbox astrometry
prop_mo_ra=6506.05 |
| radial_v = +245.2<ref name="aaa418_989"/>
prop_mo_dec=-5731.39 |
| prop_mo_ra = +6,505.08<ref name="aaa474_2_653"/>
parallax=255.27 |
| prop_mo_dec = -5,730.84<ref name="aaa474_2_653"/>
p_error=0.86 |
| parallax = 255.66
absmag_v=10.88 }}
| p_error = 0.91
{{Starbox detail|
| parallax_footnote = <ref name="aaa474_2_653"/>
mass=0.38 |
| absmag_v =
radius=0.24 |
}}
luminosity=0.004 |
{{Starbox detail
temperature=3,800 |
| mass = 0.274<ref name="Kotoneva"/>
metal=32% |
| radius = {{nowrap|0.291 ± 0.025}}<ref name="aaa505_1_205"/>
rotation= |
| gravity = 4.96<ref name="Kotoneva"/>
age=? }}
| luminosity =
{{Starbox catalog |
| temperature = 3,570<ref name=Kotoneva/>
names=VZ Pictoris, [[Gliese-Jahreiss catalogue|GJ]] 191, [[Henry Draper catalogue|HD]] 33793, [[Cordoba Durchmusterung|CD]]-45°1841, CP(D)-44°612, SAO 217223, [[Luyten Half-Second catalogue|LHS]] 29, [[Luyten Two-Tenths catalogue|LTT]] 2200, [[Luyten Five-Tenths catalogue|LFT]] 395, [[Cordoba Durchmusterung|CD]] [[General Catalogue of Trigonometric Parallaxes|GCTP]] 1181, UGPMF 628, [[Hipparcos catalogue|HIP]] 24186.}}
| metal_fe = {{nowrap|–0.99 ± 0.04}}<ref name="mnras356_3_963"/>
| rotational_velocity = 9.15<ref name="mnras407_3_1657"/>
| age_gyr = ~10<ref name="Kotoneva"/>
}}
{{Starbox catalog
| names=VZ Pictoris, [[格利泽近星星表|GJ]] 191, [[HD星表|HD]] 33793, [[波恩星表|CD]]-45°1841, CP(D)-44°612, SAO 217223, [[Luyten Half-Second catalogue|LHS]] 29, [[Luyten Two-Tenths catalogue|LTT]] 2200, [[Luyten Five-Tenths catalogue|LFT]] 395, [[General Catalogue of Trigonometric Parallaxes|GCTP]] 1181, [[依巴谷卫星|HIP]] 24186.<ref name="SIMBAD"/>
}}
{{Starbox reference
| Simbad = NAME+Kapteyn's+star
| EPE=
| ARICNS = <!--Code-->
}}
{{Starbox end}}
{{Starbox end}}


'''卡普坦星'''（'''Kapteyn's Star'''）也稱為'''GJ 191'''、'''HD 33793'''或'''CD -45 1841'''，位於[[繪架座]]，是一顆[[次矮星]]，由[[雅各布斯·卡普坦]]於1897年所發現，距離[[太陽]]僅12.79[[光年]]。
'''卡普坦星'''（'''Kapteyn's Star'''）也稱為'''GJ 191'''、'''HD 33793'''或'''CD -45 1841'''，位於[[繪架座]]，是一顆[[恆星光譜|光譜型]] M1 的[[次矮星]]，由[[雅各布斯·卡普坦]]於1897年所發現，距離[[太陽]]僅12.79[[光年]]。該恆星視星等9等，必須以望遠鏡觀測<ref name="SIMBAD"/>。


卡普坦星被發現時是當時已知[[自行運動]]最大的恆星，超過[[葛羅姆布里吉1830]]，不過後來發現的[[巴納德星]]自行運動的速度則進一步超過卡普坦星。
卡普坦星被發現時是當時已知[[自行運動]]最大的恆星，超過[[葛羅姆布里吉1830]]，不過後來發現的[[巴納德星]]自行運動的速度則進一步超過卡普坦星。

==觀測歷史==
卡普坦星是由[[荷蘭]]天文學家[[雅各布斯·卡普坦]]發現於1898年<ref name="an145_9_159"/>。當卡普坦重新檢視[[星圖]]和攝影板時，發現卡普坦星的[[自行]]極高，每年在天球上移動超過8[[角秒]]。稍後卡普坦星正式被命名以對卡普坦的貢獻致敬<ref name="kaler"/>。卡普坦星被發現時是當時已知自行最大的恆星，超過[[葛羅姆布里吉1830]]。 不過於1916年發現的[[巴納德星]]自行速度則進一步超過卡普坦星<ref name="EEB"/><ref name="Kotoneva"/><ref name="kaler"/>。2014年天文學家宣布在卡普坦星旁發現兩個[[超級地球]]候選天體<ref name="planets"/>。

==特徵==
Based upon [[parallax]] measurements with the [[Hipparcos]] astrometry satellite,<ref name="aaa474_2_653"/> Kapteyn's Star is at a distance of {{Convert|12.76|ly|pc|abbr=off|lk=on}} from the [[Earth]].<ref name="aaa474_2_653"/> It came within {{Convert|7.00|ly|pc|abbr=off}} of the [[Sun]] about 10,800 years ago and has been moving away since that time.<ref name="al36_3_220"/> The star is between one quarter and one third the size and mass of the Sun and much cooler at about 3500&nbsp;°K, with some disagreement in the exact measurements between different observers.<ref name="Kotoneva"/> The [[stellar classification]] is sdM1,<ref name="mnras403_4_1949"/> which indicates that it is a [[subdwarf star]] with a luminosity lower than that of a [[main sequence]] star at the same spectral type of M1. The abundance of elements other than hydrogen and helium, what astronomers term the [[metallicity]], is about 14% of the abundance in the Sun.<ref name="mnras356_3_963"/><ref name="abundance"/> It is a [[variable star]] of the [[BY Draconis variable|BY Draconis type]] with the [[Variable star designation|identifier]] VZ Pictoris. This means that the luminosity of the star changes because of [[stellar magnetic field|magnetic activity]] in the [[chromosphere]] coupled with [[stellar rotation|rotation]] moving the resulting [[star spot]]s into and out of the line of sight with respect to the Earth.<ref name="var"/>

Kapteyn's Star is distinctive in a number of other regards: it has a high radial velocity,<ref name="kaler"/> orbits the [[Milky Way]] [[retrograde motion|retrograde]],<ref name="Kotoneva"/> and is the nearest known [[galactic halo|halo]] star to the Sun.<ref name=mnras350_2_575/> It is a member of a [[moving group]] of stars that share a common trajectory through space, named the Kapteyn moving group.<ref name=aj112_2661/> Based upon their [[Abundance of the chemical elements|element abundances]], these stars may once have been members of [[Omega Centauri]], a [[globular cluster]] that is thought to be the remnant of a [[dwarf galaxy]] that merged with the Milky Way. During this process, the stars in the group, including Kapteyn's Star, may have been stripped away as tidal debris.<ref name="Kotoneva"/><ref name="aj139_2_636"/><ref name="ns20091104"/>


==行星系統==
==行星系統==
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{{OrbitboxPlanet begin
{{OrbitboxPlanet begin
| name = Kapteyn's star
| name = 卡普坦星
| table_ref =
| table_ref =
| period_unit = day
| period_unit = day
第72行： 第91行：
==參考資料==
==參考資料==
{{reflist|30em|refs=
{{reflist|30em|refs=

<ref name="aaa474_2_653">{{citation | first=F. | last=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 |arxiv = 0708.1752 }}.</ref>

<ref name="SIMBAD">{{citation | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=NAME+Kapteyn%27s+star | title=V* VZ Pic -- Variable Star | work=SIMBAD | publisher=[[史特拉斯堡天文資料中心|Centre de Données astronomiques de Strasbourg]] | accessdate=2009-10-14}}.</ref>

<ref name="an145_9_159">{{citation | last=Kapteyn | first=J. C. | authorlink=雅各布斯·卡普坦 | title=Stern mit grösster bislang bekannter Eigenbewegung | year=1898 | journal=Astronomische Nachrichten | volume=145 | issue=9–10 | pages=159–160 | doi=10.1002/asna.18981450906 | bibcode=1897AN....145..159K }}.</ref>

<ref name="EEB">{{citation | first=E. E. | last=Barnard | authorlink=愛德華·愛默生·巴納德 | year=1916 | title=A small star with large proper motion | journal=Astronomical Journal | volume=29 | issue=695 | page=181 | bibcode = 1916AJ.....29..181B | doi = 10.1086/104156 }}.</ref>

<ref name="al36_3_220">{{citation | last=Bobylev | first=Vadim V. |date=March 2010 | 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>

<ref name="var">{{citation | url=http://www.sai.msu.su/groups/cluster/gcvs/cgi-bin/search.cgi?search=VZ+pic | title=VZ Pic | work=[[變星總表|General Catalogue of Variable Stars]], [[斯特恩伯格天文研究所|Sternberg Astronomical Institute]], Moscow, Russia | accessdate=2009-10-14 }}</ref>

<ref name="Kotoneva">{{citation | display-authors=1 | first1=E. | last1=Kotoneva | first2=K. | last2=Innanen | first3=P. C. | last3=Dawson | first4=P. R. | last4=Wood | first5=M. M. | last5=De Robertis | title=A study of Kapteyn's star | year=2005 | journal=Astronomy & Astrophysics | volume=438 | pages=957–962 | doi=10.1051/0004-6361:20042287 | bibcode=2005A&A...438..957K | issue=3 }}.</ref>

<ref name="ns20091104">{{citation | url=http://www.newscientist.com/article/mg20427334.100-backward-star-aint-from-round-here.html | title=Backward star ain't from round here | journal=[[New Scientist]] | date=November 4, 2009 }}</ref>

<ref name="mnras350_2_575">{{citation | doi=10.1111/j.1365-2966.2004.07671.x | title=Chemical abundance analysis of Kapteyn's Star | last1=Woolf | first1=V. M. | last2=Wallerstein | first2=G. | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=350 | issue=2 | pages=575–579 | year=2004 | bibcode=2004MNRAS.350..575W }}.</ref>

<ref name="kaler">{{citation | contribution=Kapteyn's Star | pages=108–109 | title=The Hundred Greatest Stars | first=James B. | last=Kaler | publisher=Copernicus Books | year=2002 }}.</ref>

<ref name="aaa418_989">{{citation | display-authors=1 | last1=Nordström | first1=B. | last2=Mayor | first2=M. | last3=Andersen | first3=J. | last4=Holmberg | first4=J. | last5=Pont | first5=F. | last6=Jørgensen | first6=B. R. | last7=Olsen | first7=E. H. | last8=Udry | first8=S. | last9=Mowlavi | first9=N. | title=The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs | journal=Astronomy and Astrophysics | volume=418 | pages=989–1019 |date=May 2004 | doi=10.1051/0004-6361:20035959 | bibcode=2004A&A...418..989N| issue=3 | arxiv=astro-ph/0405198 }}</ref>

<ref name="aj112_2661">{{citation | last1=Eggen | first1=O. J. | title=The Ross 451 Group of Halo Stars | journal=Astronomical Journal | volume=112 | page=2661 |date=December 1996 | bibcode=1996AJ....112.2661E |doi = 10.1086/118210 }}</ref>

<ref name="aj139_2_636">{{citation | last1=Wylie-de Boer | first1=Elizabeth | last2=Freeman | first2=Ken | last3=Williams | first3=Mary | title=Evidence of Tidal Debris from ω Cen in the Kapteyn Group | journal=The Astronomical Journal | volume=139 | issue=2 | pages=636–645 |date=February 2010 | doi=10.1088/0004-6256/139/2/636 | bibcode=2010AJ....139..636W |arxiv = 0910.3735 }}</ref>

<ref name="mnras407_3_1657">{{citation | last1=Houdebine | first1=E. R. | title=Observation and modelling of main-sequence star chromospheres - XIV. Rotation of dM1 stars | journal=Monthly Notices of the Royal Astronomical Society | volume=407 | issue=3 | pages=1657–1673 |date=September 2010 | doi=10.1111/j.1365-2966.2010.16827.x | bibcode=2010MNRAS.407.1657H }}</ref>

<ref name="mnras403_4_1949">{{citation | display-authors=1 | last1=Koen | first1=C. | last2=Kilkenny | first2=D. | last3=van Wyk | first3=F. | last4=Marang | first4=F. | title=UBV(RI)<sub>C</sub> JHK observations of Hipparcos-selected nearby stars | journal=Monthly Notices of the Royal Astronomical Society | volume=403 | issue=4 | pages=1949–1968 |date=April 2010 | doi=10.1111/j.1365-2966.2009.16182.x | bibcode=2010MNRAS.403.1949K }}</ref>

<ref name="mnras356_3_963">{{citation | last1=Woolf | first1=Vincent M. | last2=Wallerstein | first2=George | title=Metallicity measurements using atomic lines in M and K dwarf stars | journal=Monthly Notices of the Royal Astronomical Society | volume=356 | issue=3 | pages=963–968 |date=January 2005 | doi=10.1111/j.1365-2966.2004.08515.x | bibcode=2005MNRAS.356..963W |arxiv = astro-ph/0410452 }}</ref>

<ref name="abundance">The abundance is given by taking the metallicity to the power of 10. From Woolf and Wallerstein (2005), [M/H] ≈ –0.86 dex. Thus:
: 10<sup>–0.86</sup> = 0.138</ref>

<ref name="aaa505_1_205">{{citation | display-authors=1 | last1=Demory | first1=B.-O. | last2=Ségransan | first2=D. | last3=Forveille | first3=T. | last4=Queloz | first4=D. | last5=Beuzit | first5=J.-L. | last6=Delfosse | first6=X. | last7=di Folco | first7=E. | last8=Kervella | first8=P. | last9=Le Bouquin | first9=J.-B. | title=Mass-radius relation of low and very low-mass stars revisited with the VLTI | journal=Astronomy and Astrophysics | volume=505 | issue=1 | pages=205–215 |date=October 2009 | doi=10.1051/0004-6361/200911976 | bibcode=2009A&A...505..205D |arxiv = 0906.0602 }}</ref>


<ref name="planets">{{citation|arxiv=1406.0818|title=Two planets around Kapteyn's star : a cold and a temperate super-Earth orbiting the nearest halo red-dwarf | display-authors=1|first1=Guillem|last1=Anglada-Escudé|first2= Pamela|last2=Arriagada|first3= Mikko|last3=Tuomi|first4= Mathias|last4=Zechmeister|year=2014}}<!-- Only the first author will be shown. The first four authors are kept so that harv linking is correct; the many remaining authors are deliberately omitted. --></ref>
<ref name="planets">{{citation|arxiv=1406.0818|title=Two planets around Kapteyn's star : a cold and a temperate super-Earth orbiting the nearest halo red-dwarf | display-authors=1|first1=Guillem|last1=Anglada-Escudé|first2= Pamela|last2=Arriagada|first3= Mikko|last3=Tuomi|first4= Mathias|last4=Zechmeister|year=2014}}<!-- Only the first author will be shown. The first four authors are kept so that harv linking is correct; the many remaining authors are deliberately omitted. --></ref>

2014年6月10日 (二) 16:29的版本

卡普坦星
紅點是卡普坦星在繪架座的位置。
觀測資料
曆元 J2000
星座 繪架座
星官
赤經 05h 11m 40.58112s[1]
赤緯 -45° 01′ 06.2899″[1]
視星等（V） 8.853[2]
特性
光谱分类sdM1[2]
U−B 色指数+1.21[3]
B−V 色指数+1.57[3]
变星类型天龍座BY型變星[4]
天体测定
徑向速度 (Rv)+245.2[5] km/s
自行 (μ) 赤经：+6,505.08[1] mas/yr
赤纬：-5,730.84[1] mas/yr
视差 (π)255.66 ± 0.91[1] mas
距离12.76 ± 0.05 ly
(3.91 ± 0.01 pc)
詳細資料
質量0.274[6] M☉
半徑0.291 ± 0.025[7] R☉
表面重力 (log g)4.96[6]
溫度3,570[6] K
金属量 [Fe/H]–0.99 ± 0.04[8] dex
自轉速度 (v sin i)9.15[9] km/s
年齡~10[6] Gyr
其他命名
VZ Pictoris, GJ 191, HD 33793, CD-45°1841, CP(D)-44°612, SAO 217223, LHS 29, LTT 2200, LFT 395, GCTP 1181, HIP 24186.[3]
參考資料庫
SIMBAD资料

卡普坦星（Kapteyn's Star）也稱為GJ 191、HD 33793或CD -45 1841，位於繪架座，是一顆光譜型 M1 的次矮星，由雅各布斯·卡普坦於1897年所發現，距離太陽僅12.79光年。該恆星視星等9等，必須以望遠鏡觀測[3]。

卡普坦星被發現時是當時已知自行運動最大的恆星，超過葛羅姆布里吉1830，不過後來發現的巴納德星自行運動的速度則進一步超過卡普坦星。

觀測歷史

卡普坦星是由荷蘭天文學家雅各布斯·卡普坦發現於1898年[10]。當卡普坦重新檢視星圖和攝影板時，發現卡普坦星的自行極高，每年在天球上移動超過8角秒。稍後卡普坦星正式被命名以對卡普坦的貢獻致敬[11]。卡普坦星被發現時是當時已知自行最大的恆星，超過葛羅姆布里吉1830。 不過於1916年發現的巴納德星自行速度則進一步超過卡普坦星[12][6][11]。2014年天文學家宣布在卡普坦星旁發現兩個超級地球候選天體[13]。

特徵

Based upon parallax measurements with the Hipparcos astrometry satellite,[1] Kapteyn's Star is at a distance of 12.76光年（3.91秒差距） from the Earth.[1] It came within 7.00光年（2.15秒差距） of the Sun about 10,800 years ago and has been moving away since that time.[14] The star is between one quarter and one third the size and mass of the Sun and much cooler at about 3500 °K, with some disagreement in the exact measurements between different observers.[6] The stellar classification is sdM1,[2] which indicates that it is a subdwarf star with a luminosity lower than that of a main sequence star at the same spectral type of M1. The abundance of elements other than hydrogen and helium, what astronomers term the metallicity, is about 14% of the abundance in the Sun.[8][15] It is a variable star of the BY Draconis type with the identifier VZ Pictoris. This means that the luminosity of the star changes because of magnetic activity in the chromosphere coupled with rotation moving the resulting star spots into and out of the line of sight with respect to the Earth.[4]

Kapteyn's Star is distinctive in a number of other regards: it has a high radial velocity,[11] orbits the Milky Way retrograde,[6] and is the nearest known halo star to the Sun.[16] It is a member of a moving group of stars that share a common trajectory through space, named the Kapteyn moving group.[17] Based upon their element abundances, these stars may once have been members of Omega Centauri, a globular cluster that is thought to be the remnant of a dwarf galaxy that merged with the Milky Way. During this process, the stars in the group, including Kapteyn's Star, may have been stripped away as tidal debris.[6][18][19]

行星系統

2014年天文學家宣布在卡普坦星旁發現兩顆超級地球卡普坦b（Kapteyn b）和卡普坦c（Kapteyn c）。卡普坦b年齡約115億年，是已知可能適居行星中最古老的[13]。兩顆恆星的公轉週期接近5:2，但軌道共振在行星被發現時尚無法證實。兩顆行星的軌道動力學積分顯示這兩顆行星正處於拱線共同旋轉的動態狀態[13]，這暗示該系統已經是長時間動態穩定狀態[20]。該行星系統發現的訊息與科幻小說作家阿拉斯泰尔·雷诺兹（英语：Alastair Reynolds）的作品「悲傷卡普坦」（Sad Kapteyn）同時公布[21]。

卡普坦星的行星系
成員
(依恆星距離) 		质量 半長軸
(AU) 		轨道周期
(天) 		離心率 傾角 半径
b >4.5 M⊕ 0.168  ± 0.005 48.616 ± 0.036 <0.4 — —
c >7.0 M⊕ 0.311  ± 0.02 121.53 ± 0.25 <0.4 — —

參考資料

  1. ^ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 van Leeuwen, F., Validation of the new Hipparcos reduction, Astronomy and Astrophysics, November 2007, 474 (2): 653–664, Bibcode:2007A&A...474..653V, arXiv:0708.1752 可免费查阅, doi:10.1051/0004-6361:20078357 .
  2. ^ 2.0 2.1 2.2 Koen, C.; et al, UBV(RI)C JHK observations of Hipparcos-selected nearby stars, Monthly Notices of the Royal Astronomical Society, April 2010, 403 (4): 1949–1968, Bibcode:2010MNRAS.403.1949K, doi:10.1111/j.1365-2966.2009.16182.x 
  3. ^ 3.0 3.1 3.2 3.3 V* VZ Pic -- Variable Star, SIMBAD (Centre de Données astronomiques de Strasbourg), [2009-10-14] .
  4. ^ 4.0 4.1 VZ Pic, General Catalogue of Variable Stars, Sternberg Astronomical Institute, Moscow, Russia, [2009-10-14] 
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  7. ^ Demory, B.-O.; et al, Mass-radius relation of low and very low-mass stars revisited with the VLTI, Astronomy and Astrophysics, October 2009, 505 (1): 205–215, Bibcode:2009A&A...505..205D, arXiv:0906.0602 可免费查阅, doi:10.1051/0004-6361/200911976 
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  15. ^ The abundance is given by taking the metallicity to the power of 10. From Woolf and Wallerstein (2005), [M/H] ≈ –0.86 dex. Thus:
    10–0.86 = 0.138
  16. ^ Woolf, V. M.; Wallerstein, G., Chemical abundance analysis of Kapteyn's Star, Monthly Notices of the Royal Astronomical Society, 2004, 350 (2): 575–579, Bibcode:2004MNRAS.350..575W, doi:10.1111/j.1365-2966.2004.07671.x .
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  21. ^ Sad Kapteyn, Science fiction story released with the announcement of planetary system, Jun 4, 2014 [2014-06-04] 

外部連結

宣布發現卡普坦星的消息

取自“https://zh.wikipedia.org/w/index.php?title=卡普坦星&oldid=31556890”