编辑“︁PSR B1257+12”︁

{{Starbox begin
| name = PSR B1257+12
}}	 
{{Starbox image
| image = [[Image:Artist's concept of PSR B1257+12 system.jpg|250px|center]]
| caption = 藝術家概念下的脈衝星PSR B1257+12和其行星。
}}
{{Starbox observe
| epoch = [[J2000.0]]
| constell = [[室女座]]
| ra = 13<sup>h</sup>00<sup>m</sup>01<sup>s</sup>
| dec = +12° 40' 57" 
| appmag_v = ?
}}
{{Starbox character
| class = 中子星
| b-v = ?
| u-b = ?
| variable = 脈衝星
}} 
{{Starbox detail
| mass = 估計為1.5
| radius = ~0.00002 
| luminosity = ?
| temperature = ?
| metal = ?
| rotation = 0.006219 [[秒|s]]
| age = 3&nbsp;×&nbsp;10<sup>9</sup> <ref name=konacki>{{Cite journal|title=Masses and Orbital Inclinations of Planets in the PSR B1257+12 System|url=https://iopscience.iop.org/article/10.1086/377093|last=Konacki|first=Maciej|last2=Wolszczan|first2=Alex|date=2003-07-10|journal=[[天文物理期刊|The Astrophysical Journal]]|issue=2|doi=10.1086/377093|volume=591|pages=L147–L150|language=en|issn=0004-637X|bibcode=2003ApJ...591L.147K|arxiv=astro-ph/0305536|access-date=2020-10-15|archive-date=2020-10-17|archive-url=https://web.archive.org/web/20201017022405/https://iopscience.iop.org/article/10.1086/377093|dead-url=no}}</ref>
}} 
{{Starbox catalog
| names = PSR&nbsp;J1300+1240
}} 
{{Starbox end}} 

'''PSR B1257+12'''，前稱為'''PSR 1257+12'''，又稱為'''PSR J1300+1240'''，又名「巫妖星」（Lich）<ref name="IAU-CSN">{{cite web|url=http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt|title=IAU Catalog of Star Names|accessdate=2018-12-16|archivedate=2016-08-12|archiveurl=https://web.archive.org/web/20160812092144/http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt|dead-url=yes}}</ref>，是一顆位於[[室女座]]的[[脈衝星]]，距離[[太陽]]大約2,300[[光年]]<ref>{{cite news |title=PSR B1257+12 b: een exoplaneet rond een zombie-ster |url=https://www.scientias.nl/psr-b125712-b-een-exoplaneet-rond-een-zombie-ster/ |accessdate=2021-08-29 |work=Scientias.nl |date=2021-08-29 |language=nl |archive-date=2021-08-29 |archive-url=https://web.archive.org/web/20210829083034/https://www.scientias.nl/psr-b125712-b-een-exoplaneet-rond-een-zombie-ster/ }}</ref>。

這顆脈衝星受到注意的地方，在於它擁有一[[行星系]]，現時已知有三顆行星圍繞其運行，這些行星也是首批被發現的[[太陽系外行星]]。<ref>{{cite journal|url=http://www.naic.edu/~newslet/no33/NAICNo33.pdf|format=PDF|author=Salter, C.|title=Radio Astronomy Highlights|journal=Arecibo Newsletter|issue=33|year=2001|accessdate=2009-06-23|archive-date=2008-12-19|archive-url=https://web.archive.org/web/20081219192204/http://www.naic.edu/~newslet/no33/NAICNo33.pdf|dead-url=yes}}</ref>

這顆脈衝星最先於1990年由[[波蘭]]天文學家[[亞歷山大·沃爾茲森]]，於1990年以位於[[波多黎各]]阿雷西博的射電望遠鏡發現的。它屬於[[毫秒脈衝星]]，為[[中子星]]的一種，自轉週期為6.22毫秒，但他卻發現其脈衝信號出現不尋常，遂對它作更深入的觀測。<ref>{{Cite journal|title=Timing Observations of Four Millisecond Pulsars with the Arecibo and Effelsberg Radio Telescopes|url=https://iopscience.iop.org/article/10.1086/308206|last=Wolszczan|first=A.|last2=Doroshenko|first2=O.|date=2000-01-10|journal=[[天文物理期刊|The Astrophysical Journal]]|issue=2|doi=10.1086/308206|volume=528|pages=907–912|language=en|issn=0004-637X|last3=Konacki|first3=M.|last4=Kramer|first4=M.|last5=Jessner|first5=A.|last6=Wielebinski|first6=R.|last7=Camilo|first7=F.|last8=Nice|first8=D. J.|last9=Taylor|first9=J. H.|access-date=2020-10-15|archive-date=2020-10-18|archive-url=https://web.archive.org/web/20201018081405/https://iopscience.iop.org/article/10.1086/308206|dead-url=no}}</ref>

== 行星 ==
{{OrbitboxPlanet begin|table_ref=<ref name=konacki/>}}
{{OrbitboxPlanet
| exoplanet = [[PSR B1257+12 A|A]]
| mass_earth = 0.020 ± 0.002
| period = 25.262 ± 0.003
| semimajor = 0.19
| eccentricity = 0.0
| inclination = ~50
}}
{{OrbitboxPlanet
| exoplanet = [[PSR B1257+12 B|B]]
| mass_earth = 4.3 ± 0.2
| period = 66.5419 ± 0.0001
| semimajor = 0.36
| eccentricity = 0.0186 ± 0.0002
| inclination = 53
}}
{{OrbitboxPlanet
| exoplanet = [[PSR B1257+12 C|C]]
| mass_earth = 3.9 ± 0.2
| period = 98.2114 ± 0.0002
| semimajor = 0.46
| eccentricity = 0.0252 ± 0.0002
| inclination = 47
}}
{{Orbitbox end}}

[[File:PSR B1257+12 System.jpg|thumb|right|藝術家概念下的依照大小和軌道距離排序的PSR B1257+12行星]]

1992年，沃爾茲森與加拿大天文學家[[戴爾·弗雷]]一同發現有兩顆行星圍繞這顆脈衝星公轉，它們是首批被發現的[[脈衝星行星]]和[[系外行星]]<ref>{{cite web|url=http://www.astro.psu.edu/users/alex/pulsar_planets.htm|title=Pulsar Planets|dead-url=yes|archiveurl=https://web.archive.org/web/20051230112904/http://www.astro.psu.edu/users/alex/pulsar_planets.htm|archivedate=2005-12-30|accessdate=2011-09-27}}</ref><ref>{{Cite journal|title=A planetary system around the millisecond pulsar PSR1257 + 12|url=http://www.nature.com/articles/355145a0|last=Wolszczan|first=A.|last2=Frail|first2=D. A.|date=1992-01|journal=[[自然 (期刊)|Nature]]|issue=6356|doi=10.1038/355145a0|volume=355|pages=145–147|language=en|issn=0028-0836|access-date=2020-10-15|archive-date=2021-02-08|archive-url=https://web.archive.org/web/20210208045309/https://www.nature.com/articles/355145a0|dead-url=no}}</ref>，當時的天文學家一般認為，行星應只會在[[主序星]]周圍找到，加上另一顆脈衝星[[PSR 1829-10|PSR B1829−10]]因-{}-數據計算錯誤，而被推翻其存在行星的說法，因此人們仍對脈衝星行星存在的可能性抱持懷疑態度。及後，人們又找到第三顆繞PSR 1257+12公轉的[[行星]]，又認為它存在[[小行星帶]]或[[柯伊伯帶|古柏帶]]。<ref>{{Cite journal|title=Confirmation of Earth-Mass Planets Orbiting the Millisecond Pulsar PSR B1257 + 12|url=https://www.sciencemag.org/lookup/doi/10.1126/science.264.5158.538|last=Wolszczan|first=A.|date=1994-04-22|journal=[[科学 (期刊)|Science]]|issue=5158|doi=10.1126/science.264.5158.538|volume=264|pages=538–542|language=en|issn=0036-8075|pmid=17732735|bibcode=1994Sci...264..538}}</ref>

這三顆行星及後得以證實，人們推測它們是氣體行星剩下的岩石內核，或是恆星經超新星爆炸後，第二輪形成的行星。<ref>{{Cite journal|title=Planet formation scenarios|url=http://adsabs.harvard.edu/abs/1993ASPC...36..149P|last=Podsiadlowski|first=Philipp|date=1993-01-01|volume=36|pages=149–165|journal=|access-date=2013-12-02|archive-date=2007-11-20|archive-url=https://web.archive.org/web/20071120060149/http://adsabs.harvard.edu/abs/1993ASPC...36..149P|dead-url=no}}</ref>如果它們原先是大型氣體行星，它們應擁有較大的岩石內核，在超新星爆炸後，它們的大氣被衝擊波吹走，其剩餘岩核的軌道也漸漸與恆星接近。<ref>{{Cite journal|title=Planets orbiting Quark Nova compact remnants|url=http://www.aanda.org/10.1051/0004-6361:20030957|last=Keränen|first=P.|last2=Ouyed|first2=R.|date=2003-09|journal=[[天文与天体物理学报|Astronomy & Astrophysics]]|issue=3|doi=10.1051/0004-6361:20030957|volume=407|pages=L51–L54|issn=0004-6361|bibcode=2003A&A...407L..51K|arxiv=astro-ph/0301574}}</ref>

2005年，[[美國]][[普林斯頓大學]]天文學家{{link-en|馬克·丘赫內爾|Marc Kuchner}}認為，這些行星的內部可能富含[[碳]]元素，在強大的內部壓力下，這些碳元素也變成[[鑽石]]。<ref>{{Cite web|title=All about PSR B1257 12 - redOrbit|url=http://www.redorbit.com/topics/psr-b1257-12/|accessdate=2013-12-02|archiveurl=https://web.archive.org/web/20131203004718/http://www.redorbit.com/topics/psr-b1257-12/|archivedate=2013-12-03|dead-url=no}}</ref>

這些行星最初以大寫A至D來表示，有別於一般日外行星以“b”開始的英文小寫排序，脈衝星是以日距作排列次序，由近至遠，與其他恆星以發現時間來排列的方式不同。<ref name=konacki/>

{{clear}}

=== PSR B1257+12 A ===
{{Planetbox begin
| name = PSR B1257+12A
}}
{{Planetbox image
| image = Exoplanet Comparison PSR B1257+12 A.png
| caption = PSR B1257+12 A 和地球體積比較
}}
{{Planetbox star
| star = [[PSR B1257+12]]
| constell = [[室女座]]
| RA = {{RA|13|00|01}}
| DEC = {{DEC|+12|40|57}}
| dist_ly = 980
| dist_pc = 300
| class = 脈衝星
| mass = assumed 1.4
| radius = ~0.00002
| age = 0.8
}}
{{Planetbox orbit
| semimajor = 0.19<ref name="konacki2003">{{cite journal | url=http://www.iop.org/EJ/article/1538-4357/591/2/L147/17269.html | author=Konacki, M., Wolszczan, A. | title=Masses and Orbital Inclinations of Planets in the PSR B1257+12 System | journal=The [[天文物理期刊|Astrophysical Journal]] | volume=591 | issue=2 | pages=L147–L150 | year=2003 | doi=10.1086/377093 | bibcode=2003ApJ...591L.147K | arxiv=astro-ph/0305536 | access-date=2011-10-16 | archive-date=2020-01-04 | archive-url=https://web.archive.org/web/20200104010006/http://www.iop.org/EJ/article/1538-4357/591/2/L147/17269.html | dead-url=no }}</ref>
| eccentricity = 0.0<ref name="konacki2003"/>
| period = 25.262 ± 0.003<ref name="konacki2003"/>
| t_peri = 2,449,765.6 ± 0.2<ref name="konacki2003"/>
| inclination = 50<ref name="konacki2003"/><ref group="note" name="inclination">其軌道傾角是基於系統中另兩顆行星傾角分別為 53° 和 47°，而推定是 50°。引述質量是基於這假設的傾角。</ref>
}}
{{Planetbox character
| mass_earth = 0.020 ± 0.002<ref name="konacki2003"/><ref group="note" name="inclination"/>
}}
{{Planetbox discovery
| discovery_date = 1994年4月22日
| discoverers = [[亞歷山大·沃爾茲森]]
| discovery_method = 脈衝星計時法
| discovery_site = {{flag|Poland}}
| discovery_status = 已发表
}}
{{Planetbox reference
| star = PSR+1257%2B12
| planet = b
}}
{{Planetbox end}}
'''[[PSR B1257+12 A]]'''（{{lang|en|'''PSR B1257+12 b'''}}）又名'''屍鬼星'''，處於最接近脈衝星的位置，平均日距為0.19天文單位，其質量約為[[月球]]的兩倍，半徑約1400公里，公轉週期為25.262天，表面溫度約1763K。<ref name="konacki2003">{{Cite journal|title=Masses and Orbital Inclinations of Planets in the PSR B1257+12 System|url=https://iopscience.iop.org/article/10.1086/377093|last=Konacki|first=Maciej|last2=Wolszczan|first2=Alex|date=2003-07-10|journal=[[天文物理期刊|The Astrophysical Journal]]|issue=2|doi=10.1086/377093|volume=591|pages=L147–L150|language=en|arxiv=astro-ph/0305536|bibcode=2003ApJ...591L.147K|issn=0004-637X|access-date=2020-10-15|archive-date=2020-10-17|archive-url=https://web.archive.org/web/20201017022405/https://iopscience.iop.org/article/10.1086/377093|dead-url=no}}</ref>在1997年，有觀點認為這顆行星其實並不存在，只是恆星發出的[[太陽風]]，但後來這個說法已給推翻。這顆星球在過去是人類已知質量最低的行星，僅比[[月球]]的質量大一倍<ref>{{cite press release|url=http://live.psu.edu/story/10180|title=Scientists announce smallest extra-solar planet yet discovered|year=2005|publisher=Pennsylvania State University|deadurl=yes|archiveurl=https://web.archive.org/web/20081012120754/http://live.psu.edu/story/10180|archivedate=2008-10-12|access-date=2011-09-27}}</ref>，但後來被質量與[[月球]]相若的[[克卜勒37b]]所取代。<ref name="PhysicsWorld">{{Cite web|title=Astronomers find smallest exoplanet|url=https://physicsworld.com/a/astronomers-find-smallest-exoplanet/|accessdate=2020-10-15|date=2005-02-11|work=Physics World|language=en-GB|archive-date=2020-10-16|archive-url=https://web.archive.org/web/20201016235311/https://physicsworld.com/a/astronomers-find-smallest-exoplanet/|dead-url=no}}</ref>

[[File:PSR B1257+12 A.jpg|thumb|left|250px|PSR B1257+12 A]]

{{clear}}

=== PSR B1257+12 B ===
{{Planetbox begin 
| name = PSR B1257+12B
}}
{{Planetbox image
| image = Exoplanet Comparison PSR B1257+12 B.png
| caption = Size comparison of PSR B1257+12 B with Earth and Neptune.
<br/>(Based on selected hypothetical [[:File:Exoplanet Comparison PSR B1257+12 B.png#Summary|modeled compositions]])
}}
{{Planetbox star
| star = [[PSR B1257+12]]
| constell = [[室女座]]
| RA = {{RA|13|00|01}}
| DEC = {{DEC|+12|40|57}}
| dist_ly =  980
| dist_pc = 300
| class = 脈衝星
| mass = assumed 1.4
| radius = ~0.00002
| age = 0.8
}}
{{Planetbox orbit 
| semimajor = 0.36<ref name="konacki2003">{{cite journal | url=http://www.iop.org/EJ/article/1538-4357/591/2/L147/17269.html | author=Konacki, M., Wolszczan, A. | title=Masses and Orbital Inclinations of Planets in the PSR B1257+12 System | journal=The [[Astrophysical Journal]] | volume=591 | issue=2 | pages=L147–L150 | year=2003 | doi=10.1086/377093 | bibcode=2003ApJ...591L.147K | arxiv=astro-ph/0305536 | access-date=2012-01-13 | archive-date=2020-01-04 | archive-url=https://web.archive.org/web/20200104010006/http://www.iop.org/EJ/article/1538-4357/591/2/L147/17269.html | dead-url=no }}</ref>
| eccentricity = 0.0186 ± 0.0002<ref name="konacki2003"/>
| period = 66.5419 ± 0.0001<ref name="konacki2003"/>
| arg_peri = 250.4 ± 0.6<ref name="konacki2003"/>
| t_peri = 2,449,768.1 ± 0.1<ref name="konacki2003"/>
| inclination = 53 ± 4<ref name="konacki2003"/><ref group="note">確定軌道傾角的方式包含了簡併法，因為無法確認行星是順時針或逆時針運動，軌道傾角另一個互補值是127 ± 4°。</ref>
}}
{{Planetbox character 
| mass_earth = 4.3 ± 0.2<ref name="konacki2003"/>
}} 
{{Planetbox discovery 
| discovery_date = 1992年1月22日
| discoverers = [[亞歷山大·沃爾茲森]]
| discovery_method = 脈衝星計時法
| discovery_site = {{flag|Poland}}
| discovery_status = 已出版論文
}}
{{Planetbox reference
| star = PSR+1257%2B12
| planet = c
}}
{{Planetbox end}}
'''[[PSR 1257+12 B]]'''（{{lang|en|'''PSR B1257+12 c'''}}）又名'''騷幽星'''的平均日距為0.36 AU，比行星b遠，其質量為地球的四倍以上，半徑約10500公里，公轉週期為66.5419天，表面溫度約1269-1293K。<ref name="konacki2003" />由於它的軌道與行星d的接近，兩顆行星在接近時會互向對方作出[[攝動]]，人們可觀測其軌道數據的變化，這已證明了行星c和d的存在。<ref>{{Cite journal|title=A planetary system around the millisecond pulsar PSR1257 + 12|url=http://www.nature.com/articles/355145a0|last=Wolszczan|first=A.|last2=Frail|first2=D. A.|date=1992-01|journal=[[自然 (期刊)|Nature]]|issue=6356|doi=10.1038/355145a0|volume=355|pages=145–147|language=en|issn=0028-0836|bibcode=1992Natur.355..145W|access-date=2020-10-15|archive-date=2021-02-08|archive-url=https://web.archive.org/web/20210208045309/https://www.nature.com/articles/355145a0|dead-url=no}}</ref>

[[File:PSR B1257+12 B.jpg|thumb|left|280px|PSR 1257+12 B]]

{{clear}}

=== PSR B1257+12 C ===
{{Planetbox begin 
| name = PSR B1257+12C
}}
{{Planetbox image
| image = Exoplanet Comparison PSR B1257+12 C.png
| caption = Size comparison of PSR B1257+12 C with Earth and Neptune.
<br/>(Based on selected hypothetical [[:File:Exoplanet Comparison PSR B1257+12 C.png#Summary|modeled compositions]])  
}}
{{Planetbox star
| star = [[PSR B1257+12]]
| constell = [[室女座]]
| RA = {{RA|13|00|01}}
| DEC = {{DEC|+12|40|57}}
| dist_ly =  980
| dist_pc = 300
| class = 脈衝星
| mass = assumed 1.4
| radius = ~0.00002
| age = 0.8
}}
{{Planetbox orbit 
| semimajor = 0.46<ref name="konacki2003">{{cite journal | url=http://www.iop.org/EJ/article/1538-4357/591/2/L147/17269.html | author=Konacki, M., Wolszczan, A. | title=Masses and Orbital Inclinations of Planets in the PSR B1257+12 System | journal=The [[Astrophysical Journal]] | volume=591 | issue=2 | pages=L147–L150 | year=2003 | doi=10.1086/377093 | bibcode=2003ApJ...591L.147K | arxiv=astro-ph/0305536 | access-date=2012-01-13 | archive-date=2020-01-04 | archive-url=https://web.archive.org/web/20200104010006/http://www.iop.org/EJ/article/1538-4357/591/2/L147/17269.html | dead-url=no }}</ref>
| eccentricity = 0.0252 ± 0.0002<ref name="konacki2003"/>
| period = 98.2114 ± 0.0002<ref name="konacki2003"/>
| arg_peri = 108.3 ± 0.5<ref name="konacki2003"/>
| t_peri = 2,449,766.5 ± 0.1<ref name="konacki2003"/>
| inclination = 47 ± 3<ref name="konacki2003"/><ref group="note">確定軌道傾角的方式包含了簡併法，因為無法確認行星是順時針或逆時針運動，軌道傾角另一個互補值是133 ± 3°。</ref>
}}
{{Planetbox character 
| mass_earth = 3.9 ± 0.2<ref name="konacki2003"/>
}} 
{{Planetbox discovery 
| discovery_date = 1992年1月22日
| discoverers = [[亞歷山大·沃爾茲森]]
| discovery_method = 脈衝星計時法
| discovery_site = {{flag|Poland}}
| discovery_status = 已出版論文
}}
{{Planetbox reference
| star = PSR+1257%2B12
| planet = d
}}
{{Planetbox end}}
'''[[PSR 1257+12 C]]'''（{{lang|en|'''PSR B1257+12 d'''}}）又名'''梦星'''的平均日距為0.46 AU，比行星B遠0.1 AU，質量約為地球3.9倍，半徑約為9800公里，其公轉週期為98.2114天，表面溫度約1119-1148K。<ref name="konacki2003"/>在PSR B1257+12 A於1994年被發現之前，這顆行星是人類已知質量最低的行星。儘管如此，其質量仍然大於地球3倍。<ref>{{Cite journal|title=A planetary system around the millisecond pulsar PSR1257 + 12|url=http://www.nature.com/articles/355145a0|last=Wolszczan|first=A.|last2=Frail|first2=D. A.|date=1992-01|journal=[[自然 (期刊)|Nature]]|issue=6356|doi=10.1038/355145a0|volume=355|pages=145–147|language=en|bibcode=1992Natur.355..145W|issn=0028-0836|access-date=2020-10-15|archive-date=2021-02-08|archive-url=https://web.archive.org/web/20210208045309/https://www.nature.com/articles/355145a0|dead-url=no}}</ref>

[[File:PSR B1257+12 C.jpg|thumb|left|280px|PSR B1257+12 C]]{{clear}}

===第四顆行星===
{{Planetbox begin 
| name = 未知天體
}}
{{Planetbox orbit 
| semimajor = ~2.6
| period = ~3.5
}}
{{Planetbox character 
| mass_earth = &lt;0.0004
}} 
{{Planetbox discovery 
| discovery_date = 2002
| discoverers = [[亞歷山大·沃爾茲森]]
| discovery_method = 脈衝星計時法
| discovery_site = {{flag|Poland}}
}}
{{Planetbox end}}

人們認為，系統除了上述三顆行星外，尚有其他天體存在，並以行星d來代表，估計平均日距約2.8天文單位，質量約地球的萬分之四倍，半徑約700公里，表面溫度約459K，自轉約五小時。它可能是小行星，或是一顆[[彗星]]，其可能質量上限為[[冥王星]]的0.2倍，直徑上限為1,000公里，但這個推測尚未證實。<ref>{{cite journal|title=A ''comet'' orbiting a pulsar?|author=Daniel Fischer|url=http://www.astro.uni-bonn.de/~dfischer/mirror/244.html|journal=The Cosmic Mirror|accessdate=2011-09-27|issue=244|year=2002|archiveurl=https://web.archive.org/web/20060510050114/http://www.astro.uni-bonn.de/~dfischer/mirror/244.html|archivedate=2006-05-10|dead-url=no}}</ref>

於1996年，天文學家們宣佈他們發現了一個類似[[土星]]的[[類木行星|氣體巨行星]]圍繞著脈衝星公轉，其半長軸為40 AU。<ref>{{cite conference|last=Wolszczan|first=Alex|title=The Pulsar Planets Update|booktitle=Planets Beyond the Solar System and the Next Generation of Space Missions. Proceedings of a workshop held at Space Telescope Science Institute, Baltimore, MD, October 16-18, 1996.  ASP Conference Series, Vol. 119|pages=135|publisher=[[太平洋天文学会|Astronomical Society of the Pacific]]|year=1997|url=http://adsabs.harvard.edu/full/1997ASPC..119..135W|accessdate=02.03.2013}}</ref>但是，天文學家們後來卻發現，其天體位置所產生的信號頻率僅局限在430 MHz，並非如一般行星會產生任何頻率的信號，因此存在大型行星的說法被推翻，並認為其信號應是上述的小型天體造成的。他們因此宣佈該行星並非一個氣體巨行星，而是一個大小僅為[[冥王星]]1/5的[[矮行星]]，其平均半長軸為2.4 AU，公轉周期為4.6年。<ref>{{cite journal |last = Fischer |first = Daniel |title = A comet orbiting a pulsar? |journal = The Cosmic Mirror |issue = 244 |date = 2002-10-25 |url = http://www.astro.uni-bonn.de/~dfischer/mirror/244.html |accessdate = 02.03.2013 |archivedate = 2006-05-10 |archiveurl = https://web.archive.org/web/20060510050114/http://www.astro.uni-bonn.de/~dfischer/mirror/244.html |dead-url = yes }}</ref><ref>{{Cite news|title=Smallest extra-solar planet found|url=http://news.bbc.co.uk/2/hi/science/nature/4264603.stm|date=2005-02-14|accessdate=2020-10-15|language=en-GB|archive-date=2013-12-03|archive-url=https://web.archive.org/web/20131203131109/http://news.bbc.co.uk/2/hi/science/nature/4264603.stm|dead-url=no}}</ref><ref name="Wolszczan2012">{{Cite journal|title=Discovery of pulsar planets|url=https://linkinghub.elsevier.com/retrieve/pii/S1387647311000418|last=Wolszczan|first=Alex|date=2012-01|journal=New Astronomy Reviews|issue=1|doi=10.1016/j.newar.2011.06.002|volume=56|pages=2–8|language=en|bibcode=2012NewAR..56....2W|access-date=2020-10-15|archive-date=2020-09-04|archive-url=https://web.archive.org/web/20200904052857/https://linkinghub.elsevier.com/retrieve/pii/S1387647311000418|dead-url=no}}</ref>諷刺的是，矮行星的說法後來又被收回，全因「該星球的公轉並非週期性的，因此未能肯定其外貌與特質」。<ref name="Wolszczan2012" />

{{clear}}

== 請參閱 ==
* [[太陽系外行星]]
* [[脈衝星行星]]
* [[碳行星]]

== 參考資料 ==
{{Reflist|2}}

== 相關網站 ==
{{commons|Category:PSR B1257+12 A|PSR B1257+12 A}}
{{commons|Category:PSR B1257+12 B|PSR B1257+12 B}}
{{commons|Category:PSR B1257+12 C|PSR B1257+12 C}}

* [http://solar.starparadise.net/html/solar_system/other.htm 其他太阳系]{{Wayback|url=http://solar.starparadise.net/html/solar_system/other.htm |date=20060103165614 }}
* [https://web.archive.org/web/20060504222106/http://database.cpst.net.cn/popul/views/artic/50220155911.html 中国公众科技网：宇宙中可能存在钻石行星]
*[https://web.archive.org/web/20051230112904/http://www.astro.psu.edu/users/alex/pulsar_planets.htm Pulsar Planets]
*[https://web.archive.org/web/20080525161540/http://exoplanet.eu/star.php?st=PSR+1257+12 PSR 1257+12] on ''[https://web.archive.org/web/20080613163808/http://exoplanet.eu/index.php The Extrasolar Planets Encyclopaedia]''
*{{Cite web|title=Found! First Earth-Size Planet That Could Support Life|url=https://www.space.com/25530-earthsize-exoplanet-kepler-186f-habitable-discovery.html|accessdate=2020-10-15|last=April 2014|first=Miriam Kramer 17|work=Space.com|language=en|archive-date=2020-12-07|archive-url=https://web.archive.org/web/20201207215424/https://www.space.com/25530-earthsize-exoplanet-kepler-186f-habitable-discovery.html|dead-url=no}}

{{PSR B1257+12}}
[[Category:太陽系外行星]]
[[Category:室女座]]
[[Category:脈衝星]]
[[Category:波兰科技]]