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{{noteTA
|1=zh-hans:超新星遗迹; zh-hant:超新星爆炸遺骸;
}}
{{Starbox begin
|name=SS 433
}}
{{Starbox image
|image=[[File:Ss433 art big.gif|250px]]
|caption=藝術家想像下的SS 433
}}
{{Starbox observe
|epoch=[[J2000.0]] ([[國際天球參考系|ICRS]])
|constell=[[天鷹座]]
|ra={{RA|19|11|49.56}}<ref name=dr2/>
|dec={{DEC|+04|58|57.8}}<ref name=dr2/>
|appmag_v=13.0 - 17.3<ref name=gcvs/>
}}
{{Starbox character |
class=A7Ib |
r-i = |
v-r = |
b-v = |
u-b = |
variable=[[聯星|食雙星]]<ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1|pages=B/gcvs|display-authors=etal|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref>
}}
{{Starbox astrometry
| radial_v=
| prop_mo_ra= -2.853
| prop_mo_dec= -4.570
| parallax= 0.2161
| p_error= 0.0626
| parallax_footnote = <ref name=dr2>{{cite DR2|4293406612283985024}}</ref>
| dist_pc={{val|5500|200|fmt=commas}}<ref name="asym">{{cite journal|last1=Blundell|first1=Katherine M.|author-link1=Katherine Blundell|last2=Bowler|first2=Michael G.|title=Symmetry in the Changing Jets of SS 433 and Its True Distance from Us|journal=[[The Astrophysical Journal]]|volume=616|issue=2|year=2004|pages=L159–L162|issn=0004-637X|doi=10.1086/426542|arxiv=astro-ph/0410456|bibcode=2004ApJ...616L.159B|s2cid=11213274}}</ref><ref name=jeffphd>{{cite thesis|degree=DPhil|publisher=University of Oxford|url=https://ora.ox.ac.uk/objects/uuid:b9f5657b-a122-464f-8c55-db349ba74c4c|title=The remarkable outflows from the galactic microquasar SS433|first=Robert|last=Jeffrey|date=2016|id={{EThOS|uk.bl.ethos.730205}}|website=ora.ox.ac.uk|access-date=2022-07-21|archive-date=2020-10-25|archive-url=https://web.archive.org/web/20201025060654/https://ora.ox.ac.uk/objects/uuid:b9f5657b-a122-464f-8c55-db349ba74c4c|dead-url=no}} {{free access}}</ref>
| dist_ly={{val|18,000|700|fmt=commas}}
| absmag_v=
}}
{{Starbox orbit
|reference=<ref name=Cherepashchuk>{{cite journal|doi=10.1093/mnrasl/slab083|arxiv=2107.09005|bibcode=2021MNRAS.507L..19C|title=Discovery of orbital eccentricity and evidence for orbital period increase of SS433|year=2021|last1=Cherepashchuk|first1=A. M.|last2=Belinski|first2=A. A.|last3=Dodin|first3=A. V.|last4=Postnov|first4=K. A.|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=507|issue=1|pages=L19–L23}}</ref>
|period_unitless=13.082 d
|eccentricity=0.05 ± 0.01
|inclination=79
}}
{{Starbox catalog
|names=V1343 Aql、[[GAL (astronomical catalogue)|GAL]] 039.7-02.0、[[2微米全天巡天|2MASS]] J19114957+0458578、[[美國海軍天文台|USNO]] 659, 1A 1909+04、[[87GB]] 190920.8+045332、[[NEK (astronomical catalogue)|NEK]] 40.1-02.1、[[List of astronomical catalogues#0-9|3A]] 1909+048、[[全球定位系統|GPS]] 1909+049、[[三原色光模式|RGB]] J1911+049、BWE 1909+0453, [[GRS (astronomical catalogue)|GRS]] 039.60 -01.80、[[倫琴衛星|RX]] J1911.7+0459、[[4C星表]]04.66、[[1H (astronomical catalogue)|1H]] 1908+047、[[1RXS]] J191149.7+045857、[[愛因斯坦衛星|2E]] 1909.3+0453、 [[HBHA]] 204-02、[[美國變星觀測者協會]] 1906+04、[[愛因斯坦衛星|2E]] 4204、[[國際伽瑪射線天體物理實驗室|INTEGRAL1]] 110、[[TXS]] 1909+048、[[1ES]] 1909+04.8、[[INTREF]] 969、[[4U (astronomical catalogue)|4U]] 1908+05。}}
{{Starbox reference | Simbad=SS+433}}
{{Starbox end}}

[[File:SS433LightCurve.png|thumb|改編自Watarai & Fukue（2010）的SS 433在[[測光系統#使用中的濾鏡系統|可見光]]波段的[[光變曲線]]<ref name="Watarai"/>。]]

'''SS 433'''是觀測到的最奇特[[恆星系統]]之一。它位於[[銀河系]]，並且是一個[[食雙星]]、[[X射線聯星]]的[[恆星系統|系統]]，主星是恆星質量的[[黑洞]]<ref name=Cherepashchuk/>，[[聯星#名稱|伴星]]的光譜表明它是一顆晚期的[[A型主序星|A型星]]<ref>{{cite journal|bibcode=2004ApJ...615..422H|title=Identification of the Mass Donor Star's Spectrum in SS 433|url=https://archive.org/details/sim_astrophysical-journal_2004-11-01_615_1/page/422|journal=The Astrophysical Journal|volume=615|issue=1|pages=422–431|last1=Hillwig|first1=T. C.|last2=Gies|first2=D. R.|last3=Huang|first3=W.|last4=McSwain|first4=M. V.|last5=Stark|first5=M. A.|last6=Van Der Meer|first6=A.|last7=Kaper|first7=L.|year=2004|doi=10.1086/423927|arxiv=astro-ph/0403634|s2cid=17930915}}</ref>。SS 433是第一個被發現的[[微類星體]]<ref name="darling" />，它位於超新星遺跡[[W50]]的中心。

SS 433的命名來自[[凱斯西儲大學]]的兩位天文學家的首字母縮寫：[[尼可拉斯·桑度列克|Nicholas Sanduleak]]和{{link-en|查爾斯·布魯斯·斯蒂芬森|Charles Bruce Stephenson}}。這是他們編輯具有強大發射線的1977顆恆星目錄中的第433個條目<ref name="darling">[http://www.daviddarling.info/encyclopedia/S/SS_433.html SS 433] {{Wayback|url=http://www.daviddarling.info/encyclopedia/S/SS_433.html |date=20080330001603 }}, David Darling, entry in ''The Internet Encyclopedia of Science'', accessed on line September 14, 2007.</ref>。

== 位置 ==
SS 433，也稱為天鷹座V1343，位於銀河系平面的5.5 kpc（''l= 39.7°和b= -2.2°''）

== 系統 ==
緻密的中心天體正在吞噬伴星，伴星迅速失去質量，形成圍繞中心天體的[[吸積盤]]。吸積盤在螺旋進入主星時受到極端加熱，這種加熱導致吸積盤沿著旋轉軸發射強烈的X射線，並向吸積盤的上方和下方射出熱氫噴流；噴流中的物質以[[光速]]的26%運動<ref name="ara" />。伴星的質量可能比主星原本的質量低，因此壽命更長。估計它的質量介於太陽質量的3至30倍<ref>{{cite journal|bibcode=2005A&A...437..561C|doi=10.1051/0004-6361:20041563|title=INTEGRAL observations of SS433: Results of a coordinated campaign|journal=Astronomy and Astrophysics|volume=437|issue=2|pages=561–573|last1=Cherepashchuk|first1=A. M.|last2=Sunyaev|first2=R. A.|last3=Fabrika|first3=S. N.|last4=Postnov|first4=K. A.|last5=Molkov|first5=S. V.|last6=Barsukova|first6=E. A.|last7=Antokhina|first7=E. A.|last8=Irsmambetova|first8=T. R.|last9=Panchenko|first9=I. E.|last10=Seifina|first10=E. V.|last11=Shakura|first11=N. I.|last12=Timokhin|first12=A. N.|last13=Bikmaev|first13=I. F.|last14=Sakhibullin|first14=N. A.|last15=Aslan|first15=Z.|last16=Khamitov|first16=I.|last17=Pramsky|first17=A. G.|last18=Sholukhova|first18=O.|last19=Gnedin|first19=Yu. N.|last20=Arkharov|first20=A. A.|last21=Larionov|first21=V. M.|year=2005|arxiv=astro-ph/0503352|s2cid=119395465}}</ref>。從恆星的角度來看，主星和伴星在非常近的距離上相互繞行，軌道週期為13.082天。它們的軌道[[軌道離心率|扁率]]非常輕微，但正以每秒{{val|1.0e-7}}角秒或每年3角秒的速率增加<ref name=Cherepashchuk/>。

== 觀測數據 ==
來自主星發射的噴流垂直於其[[吸積盤]]。喷流和吸积盘绕着一个与地球到SS433的直线呈79°的轴[[进动]]。噴流與軸線之間的夾角約為20°，進動週期約為162.5天<ref name="xxx">{{cite journal|bibcode=2002SSRv..102...23C|title=Observational Manifestations of Precession of Accretion Disk in the SS 433 Binary System|journal=Space Science Reviews|volume=102|issue=1|pages=23–35|last1=Cherepashchuk|first1=Anatol|year=2002|doi=10.1023/a:1021356630889 |s2cid=115604949}}</ref>。進動意味著噴流的指向有時朝向地球，有時遠離地球的方向，在觀察到的可見光譜中產生藍色和紅色[[都卜勒效應|都卜勒頻移]] <ref name="ara" />。此外，進動意味著噴流在膨脹的空間中通過時，在膨脹的霧氣中像螺旋開瓶器一樣的前進<ref>[http://www.nrao.edu/pr/2004/ss433corkscrew/ Gigantic Cosmic Corkscrew Reveals New Details About Mysterious Microquasar] {{Wayback|url=http://www.nrao.edu/pr/2004/ss433corkscrew/ |date=20160418085006 }}, press release, [[National Radio Astronomy Observatory]], October 26, 2004, accessed on line September 14, 2007.</ref>。當它們撞擊周圍的[[W50|超新星殘骸]]雲氣時，它們會扭曲成拉長的形狀<ref>{{cite journal|bibcode=1996PASJ...48..819M|title=Interaction of Jets with a Supernova Remnant in the SS 433/W50 System|journal=Publications of the Astronomical Society of Japan|volume=48|pages=819–825|last1=Murata|first1=Kenji|last2=Shibazaki|first2=Noriaki|year=1996|issue=6|doi=10.1093/pasj/48.6.819|doi-access=free}}</ref>。

[[File:PIA24574-SS433-ULXray-20210709.jpg|thumb|left|500px|<div align="center">SS 433 – 可能的{{link-en|超亮X射線源|Ultraluminous X-ray source}}（ULX ray source）</div>]]

2004年，[[超長基線陣列]]對SS 433進行了連續42天的觀測，獲得的數據對噴流活動有新的理解。為噴氣式飛機的行動提供了新的數據和理解。看起來，噴流有時會在創造後不久撞擊物質使它們變亮。但噴流撞擊的物質似乎在某些時候會替換，但並非總是如此，導致噴流的亮度產生變化<ref>[http://www.nrao.edu/pr/2004/ss433/ VLBA "Movie" Gives Scientists New Insights On Workings of Mysterious Microquasars] {{Wayback|url=http://www.nrao.edu/pr/2004/ss433/ |date=20120516155412 }}, press release, [[National Radio Astronomy Observatory]], January 5, 2004. Accessed online September 14, 2007.</ref><ref>{{cite journal|bibcode=2004AAS...20510401S|title=Exploring the Jet Proper Motions of SS433|journal=American Astronomical Society Meeting Abstracts|volume=205|pages=104.01|last1=Schillemat|first1=K.|last2=Mioduszewski|first2=A.|last3=Dhawan|first3=V.|last4=Rupen|first4=M.|year=2004}}</ref>。

SS 433的光譜不僅受到[[都卜勒效應|都卜勒頻移]]的影響，還受到[[狹義相對論|相對論]]的影響：當減去都卜勒頻移的影響後，還存在對應於速度大約12,000[[公里]]/[[秒]]的紅移量。這並不代表系統離開地球的實際速度；而是由於[[時間膨脹]]，使得移動的時鐘在靜止的觀察者看來滴答作響得更慢。在這種情況下，在噴流中移動的激發原子似乎振動得更慢，因此它們的輻射看起來是紅移的<ref name="ara">{{cite journal|last1=Margon|first1=Bruce|title=Observations of SS 433|journal=Annual Review of Astronomy and Astrophysics|volume=22|issue=1|year=1984|pages=507–536|issn=0066-4146|doi=10.1146/annurev.aa.22.090184.002451|bibcode=1984ARA&A..22..507M}}</ref>。

在2018年9月，A. U. Abeysekara等人在《''[[自然 (期刊)|自然]] ''》Nature （journal）|Nature]]發表使用'[[墨西哥]]的{{link-en|高海拔水切倫科夫天文臺|High Altitude Water Cherenkov Experiment}}（HAWC）的研究結果。他們報告在空間上解析了波瓣，觀察到超過25[[TeV]]的SS 433 / W50系統的太電子伏特的γ射線，並且與單個電子群一致，其能量在約16微[[高斯]]的磁場中至少擴展到數百個太電子伏特<ref>{{cite journal|doi=10.1038/s41586-018-0565-5|pmid=30283106|title=Very-high-energy particle acceleration powered by the jets of the microquasar SS 433|journal=Nature|volume=562|issue=7725|pages=82–85|year=2018|last1=Abeysekara|first1=A. U.|last2=Albert|first2=A.|last3=Alfaro|first3=R.|last4=Alvarez|first4=C.|last5=Álvarez|first5=J. D.|last6=Arceo|first6=R.|last7=Arteaga-Velázquez|first7=J. C.|last8=Avila Rojas|first8=D.|last9=Ayala Solares|first9=H. A.|last10=Belmont-Moreno|first10=E.|last11=Benzvi|first11=S. Y.|last12=Brisbois|first12=C.|last13=Caballero-Mora|first13=K. S.|last14=Capistrán|first14=T.|last15=Carramiñana|first15=A.|last16=Casanova|first16=S.|last17=Castillo|first17=M.|last18=Cotti|first18=U.|last19=Cotzomi|first19=J.|last20=Coutiño De León|first20=S.|last21=De León|first21=C.|last22=de la Fuente|first22=E.|last23=Díaz-Vélez|first23=J. C.|last24=Dichiara|first24=S.|last25=Dingus|first25=B. L.|author25-link= Brenda Dingus |last26=Duvernois|first26=M. A.|last27=Ellsworth|first27=R. W.|last28=Engel|first28=K.|last29=Espinoza|first29=C.|last30=Fang|first30=K.|display-authors=29|arxiv=1810.01892|bibcode=2018Natur.562...82A|s2cid=52918329}}</ref><ref name="2018-10-04_SD">[http://www.spacedaily.com/reports/Scientists_discover_new_nursery_for_superpowered_photons_999.html Scientists discover new nursery for superpowered photons] {{Wayback|url=http://www.spacedaily.com/reports/Scientists_discover_new_nursery_for_superpowered_photons_999.html |date=20220320075535 }}, [[Space Daily]], 2018-10-04</ref>。

== 在流行文化中 ==
在''[[週六夜現場]]''的第四季（1979年），{{link-en|圭多·薩杜奇神父|Father Guido Sarducci}}提到了SS 433.<ref>Archived at [https://ghostarchive.org/varchive/youtube/20211205/lWBhsiBMOIo Ghostarchive]{{cbignore}} and the [https://web.archive.org/web/20190712071714/https://www.youtube.com/watch?v=lWBhsiBMOIo&gl=US&hl=en Wayback Machine]{{cbignore}}: {{cite web| url = https://www.youtube.com/watch?v=lWBhsiBMOIo&t=124| title = Father Guido Sarducci on Weekend Update - SNL | website=[[YouTube]]}}{{cbignore}}</ref>。

== 相關條目 ==
* [[X射線聯星#高質量X射線聯星|高質量X射線聯星]]
{{clear}}

== 參考資料 ==
{{Reflist|colwidth=25em|refs=

<ref name="Watarai">{{cite journal |last1=Watarai |first1=Ken-ya |last2=Fukue |first2=Jun |title=Optical Light Curves of Luminous Eclipsing Black Hole X-Ray Binaries |journal=Publications of the Astronomical Society of Japan |date=25 April 2010 |volume=62 |issue=2 |pages=467–474 |doi=10.1093/pasj/62.2.467 |url=https://doi.org/10.1093/pasj/62.2.467 |access-date=22 October 2021}}</ref>

}}

== 進階讀物 ==
* [http://aladin.u-strasbg.fr/AladinPreview?-c=19+11+49.56%2B04+58+57.6&ident=V*+V1343+Aql&submit=Aladin+previewer Image SS 433]
* [https://www.desy.de/news/news_search/index_eng.html?openDirectAnchor=1887 Strange gamma-ray heartbeat puzzles scientists] {{Wayback|url=https://www.desy.de/news/news_search/index_eng.html?openDirectAnchor=1887 |date=20220721173936 }} - article with video at [[DESY]] News
{{Sky|19|11|49.56|+|04|58|57.6|18000}}

{{天鹰座恒星}}
{{Portal bar|天文學|恆星|航天|太空|太陽系}}
{{Authority control}}

{{DEFAULTSORT:SS 433}}
[[Category:恆星黑洞]]
[[Category:天鷹座]]
[[Category:微類星體]]
[[Category:食雙星]]
[[Category:以變星命名法命名的天體|天鷹座V1343]]
[[Category:A型超巨星]]

SS 433 - 版本历史

imported>InternetArchiveBot：​Add 1 book for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot

imported>InternetArchiveBot：Add 1 book for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot