Wolf 359: Perbedaan antara revisi

<span data-segmentid="264" class="cx-segment">Wolf 359 memiliki [[klasifikasi bintang]] M6.5,<ref name="mnras245_3"><cite class="citation journal">Mukai, K.; et al. (August 1990). "Spectroscopy of faint, high latitude cataclysmic variable candidates". ''[[Monthly Notices of the Royal Astronomical Society]]''. '''245''' (3): 385–391. [[Bibcode]]:[[bibcode:1990MNRAS.245..385M|1990MNRAS.245..385M]].</cite></ref> meskipun berbagai sumber mencantumkan kelas spektral M5.5,<ref name="aaa4662"><cite class="citation journal">Reiners, A.; et al. (2007). "Rapid magnetic flux variability on the flare star CN Leonis". ''Astronomy and Astrophysics''. '''466''' (2): L13–L16. [[arXiv]]:<span class="cs1-lock-free" title="Freely accessible">[//arxiv.org/abs/astro-ph/0703172 astro-ph/0703172]</span>. [[Bibcode]]:[[bibcode:2007A&A...466L..13R|2007A&#x26;A...466L..13R]]. [[Digital object identifier|doi]]:[[doi:10.1051/0004-6361:20077095|10.1051/0004-6361:20077095]].</cite></ref> M6 <ref name="RECONS2"><cite class="citation web">Staff (June 8, 2007). [http://joy.chara.gsu.edu/RECONS/ "List of the nearest 100 stellar systems"]. Research Consortium on Nearby Stars<span class="reference-accessdate">. Retrieved <span class="nowrap">2007-07-16</span></span>.</cite></ref> atau M8.<ref name="apj4512"><cite class="citation journal">Robinson, R. D.; et al. (1995). "A search for microflaring activity on dMe flare stars. I. Observations of the dM8e Star CN Leonis". ''Astrophysical Journal''. '''451''': 795–805. [[Bibcode]]:[[bibcode:1995ApJ...451..795R|1995ApJ...451..795R]]. [[Digital object identifier|doi]]:[[doi:10.1086/176266|10.1086/176266]].</cite></ref></span> <span data-segmentid="266" class="cx-segment">[[Klasifikasi bintang|Bintang tipe M]] dikenal sebagai [[katai merah]] : disebut merah karena emisi energi bintang mencapai puncak di bagian spektrum merah dan inframerah.<ref name="jones09"><cite class="citation book">Jones, Lauren V. (2009). ''Stars and galaxies''. Greenwood Guides to the Universe. ABC-CLIO. p.&nbsp;50. [[International Standard Book Number|ISBN]]&nbsp;[[Istimewa:BookSources/978-0-313-34075-8|<bdi>978-0-313-34075-8</bdi>]].</cite></ref></span> <span data-segmentid="269" class="cx-segment">Wolf 359 memiliki luminositas yang sangat rendah, memancarkan sekitar 0,1% dari [[Luminositas matahari|energi Matahari]].<ref name="aaa4474"><cite class="citation journal">Pavlenko, Ya. V.; et al. (2006). "Spectral energy distribution for GJ406". ''Astronomy and Astrophysics''. '''447''' (2): 709–717. [[arXiv]]:<span class="cs1-lock-free" title="Freely accessible">[//arxiv.org/abs/astro-ph/0510570 astro-ph/0510570]</span>. [[Bibcode]]:[[bibcode:2006A&A...447..709P|2006A&#x26;A...447..709P]]. [[Digital object identifier|doi]]:[[doi:10.1051/0004-6361:20052979|10.1051/0004-6361:20052979]].</cite></ref><ref name="jaavso30_2"><cite class="citation journal">West, Frederick R. (2002). "Letter to the Editor: the corona of CN Leonis (Gliese 406) and its possible detection at radio frequencies". ''The Journal of the American Association of Variable Star Observers''. '''30''' (2): 149–150. [[Bibcode]]:[[bibcode:2002JAVSO..30..149W|2002JAVSO..30..149W]].</cite></ref></span> <span data-segmentid="271" class="cx-segment">Jika dipindahkan ke lokasi Matahari, bintang akan muncul sepuluh kali seterang [[bulan purnama]].<ref name="borgia06"><cite class="citation book">Borgia, Michael P. (2006). ''Human vision and the night sky: hot [i.e. how] to improve your observing skills''. Patrick Moore's practical astronomy series. Springer. p.&nbsp;208. [[International Standard Book Number|ISBN]]&nbsp;[[Istimewa:BookSources/978-0-387-30776-3|<bdi>978-0-387-30776-3</bdi>]].</cite></ref></span>

[[Berkas:Wolf359.jpg|ka|jmpl|<span data-segmentid="195" class="cx-segment">Wolf 359 adalah bintang berwarna oranye yang terletak tepat di atas pusat [[Astrofotografi|astrophotograph]] 2009 ini.</span>]]

 

<span data-segmentid="284" class="cx-segment">Seluruh bintang sedang mengalami [[Zona konveksi|konveksi]], di mana energi yang dihasilkan pada inti diangkut ke permukaan oleh gerakan [[Konveksi|konvektif]] [[Plasma (wujud zat)|plasma]], bukan melalui transmisi melalui [[Zona radiasi|radiasi]].</span> <span data-segmentid="289" class="cx-segment">Sirkulasi ini mendistribusikan kembali akumulasi helium yang dihasilkan melalui [[nukleosintesis bintang]] pada inti di seluruh bintang.<ref name="cook_jewell95"><cite class="citation web">McCook, G. P.; et al. (1995). [https://web.archive.org/web/20110615064340/http://www.csc.villanova.edu/~astronom/obs95/node12.html "Fully convective M dwarfs"]. Villanova University. Archived from [http://www.csc.villanova.edu/~astronom/obs95/node12.html the original] on 2011-06-15<span class="reference-accessdate">. Retrieved <span class="nowrap">2010-05-17</span></span>.</cite></ref></span> <span data-segmentid="291" class="cx-segment">Proses ini akan memungkinkan bintang untuk tetap berada di [[deret utama]] sebagai bintang sekering [[hidrogen]] secara proporsional lebih lama daripada bintang seperti Matahari di mana helium terus menumpuk di inti.</span> <span data-segmentid="294" class="cx-segment">Dalam kombinasi dengan tingkat konsumsi hidrogen yang lebih rendah karena massanya yang rendah, konveksi akan memungkinkan Wolf 359 untuk tetap menjadi bintang urutan utama selama sekitar delapan triliun tahun.<ref name="adams04"><cite class="citation conference">Adams, Fred C.; et al. (December 2004). "Red dwarfs and the end of the main sequence". ''Gravitational Collapse: From Massive Stars to Planets''. Revista Mexicana de Astronomía y Astrofísica. pp.&nbsp;46–49. [[Bibcode]]:[[bibcode:2004RMxAC..22...46A|2004RMxAC..22...46A]].</cite></ref></span>