| 词条 | Colliding-wind binary |
| 释义 |
A colliding-wind binary is a binary star system in which the two members are massive stars that emit powerful, radiatively-driven stellar winds. The location where these two winds collide produces a strong shock front that can cause radio, X-ray and possibly synchrotron radiation emission. Wind compression in the bow shock region between the two stellar winds allows dust formation. When this dust streams away from the orbiting pair, it can form a pinwheel nebula of spiraling dust. Such pinwheels have been observed in the Quintuplet Cluster[2] The archetype of such a colliding-wind binary system is WR 140 (HD 193793), which consists of a 20 solar mass ({{Solar mass|link=y}}) Wolf-Rayet star orbiting about a {{Solar mass|50}}, spectral class O4-5 main sequence star every 7.9 years. The high orbital eccentricity of the pair allows astronomers to observe changes the colliding winds as their separation varies.[4][5] Another prominent example of a colliding-wind binary is thought to be Eta Carinae, one of the most luminous objects in the Milky Way galaxy.[6] The first colliding-wind binary to be detected in the X-ray band outside the Milky Way galaxy was HD 5980, located in the Small Magellanic Cloud.[7] See also
References1. ^1 {{cite news | first=Bob | last=Naeye | title=First X-Ray Detection of a Colliding-Wind Binary Beyond Milky Way | date=February 16, 2007 | publisher=NASA, Goddard Space Flight Center }} [1][2][3][4][5][6]2. ^1 {{cite news | first=Dave | last=Finley | date=April 11, 2005 | title=Scientists Track Collision of Powerful Stellar Winds | publisher=National Radio Astronomy Observatory | url=http://www.nrao.edu/pr/2005/wr140/ | accessdate=2011-01-14 }} 3. ^1 {{cite journal | title=The orbit and distance of WR140 |journal=Bulletin de la Societe Royale des Sciences de Liege |volume=80 |pages=658 |author1=Dougherty, S. M. |author2=Trenton, V. |author3=Beasley, A. J. |date=November 2010 | bibcode=2011BSRSL..80..658D | arxiv=1011.0779}} 4. ^1 {{cite journal | title=Is Eta Carinae a Fast Rotator, and How Much Does the Companion Influence the Inner Wind Structure? |author1=Groh, J. H. |author2=Madura, T. I. |author3=Owocki, S. P. |author4=Hillier, D. J. |author5=Weigelt, G. | journal=The Astrophysical Journal Letters | volume=716 | issue=2 | pages=L223–L228 |date=June 2010 | doi=10.1088/2041-8205/716/2/L223 | bibcode=2010ApJ...716L.223G |arxiv = 1006.4816 }} 5. ^1 {{cite journal | last=Tuthill | first=Peter | title=Pinwheels in the Quintuplet Cluster | journal=Science | date=August 18, 2006 | volume=313 | issue=5789 | page=935 | doi=10.1126/science.1128731 | url=http://www.sciencemag.org/content/313/5789/935.full | accessdate=2011-01-14 |arxiv = astro-ph/0608427 |bibcode = 2006Sci...313..935T |display-authors=etal | pmid=16917053| citeseerx=10.1.1.255.6805 }} 6. ^1 {{cite web | title = Eta Carinae: New View of a Doomed Star | url = http://chandra.harvard.edu/photo/2007/etacar/ | date = June 20, 2007 | publisher = Chandra | accessdate = 2011-01-18}} }}{{multi-star-stub}} 1 : Binary stars |
| 随便看 |
|
开放百科全书收录14589846条英语、德语、日语等多语种百科知识，基本涵盖了大多数领域的百科知识，是一部内容自由、开放的电子版国际百科全书。