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| {{other uses}} | |||
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| {{Starbox begin | |||
| | name = Rigel, Beta Ori }} | |||
| {{Starbox image | |||
| | image=]</div> | |||
| | caption=Rigel sa réaltbhuíon d’ Orion | |||
| }} | |||
| {{Starbox observe 2s | |||
| | tús ré = J2000.0 | |||
| | réaltbhuíon = ] | |||
| | fuaimniú = {{|r|aɪ|dʒ|əl}} | |||
| | cuidí 1 = A | |||
| | ceartéirí1 = {{CÉ|05|14|32.27210}} | |||
| | díochlaonadh 1 = {{Díoch|−08|12|05.8981}} | |||
| | méid fhollasach_v1 = 0.13 | |||
| | cuidí 2 = B | |||
| | ceartéirí 2 = {{CÉ|05|14|32.049}} | |||
| | díochlaonadh2 = {{Díoch|−08|12|14.78}} | |||
| | méid fhollasach_v2 = 6.67 | |||
| }} | |||
| ---------------------------------------------------------------- | |||
| '''Rigel''', also known by its ] '''Beta Orionis''' (β Ori, β Orionis), is the brightest star in the constellation ] and the ] in the night sky, with ] 0.13. The star as seen from Earth is actually a triple or quadruple star system, with the primary star (Rigel A) a blue-white supergiant that is estimated to be anywhere from 120,000 to 279,000 times as luminous as the ], depending on method used to calculate its properties. It has exhausted its core hydrogen and swollen out to between 79 and 115 times the Sun's radius. It pulsates quasi-periodically and is classified as an ]. A companion, Rigel B, is 500 times fainter than the supergiant Rigel A and visible only with a telescope. Rigel B is itself a ] system, consisting of two ] blue-white stars of spectral type B9V that are estimated to be respectively 3.9 and 2.9 times as massive as the Sun. Rigel B also appears to have a very close visual companion Rigel C of almost identical appearance. | |||
| ==Visibility== | |||
| The apparent visual magnitude of Rigel is 0.13, making it on average the seventh brightest star in the ] excluding the Sun—just fainter than ]. It is an irregular pulsating variable with a visual range of magnitude 0.05–0.18. Although Rigel has the ] "beta", it is almost always brighter than Alpha Orionis (]). Since 1943, the ] of this star has served as one of the stable anchor points by which other stars are ].<ref name=baas25_1319/> Rigel is the third most inherently ] first magnitude star after ] and Betelgeuse. Rigel has a ] (B–V) of −0.03, meaning it appears white or slightly blue-white.<ref name="csiro">{{citation | title=The Colour of Stars | date=21 December 2004 | work=Australia Telescope, Outreach and Education | publisher=Commonwealth Scientific and Industrial Research Organisation | url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html | accessdate=28 June 2014}}</ref> | |||
| Culminating at midnight on 12 December, and at 9 pm on 24 January, Rigel is most visible in winter evenings in the ] and summer in the southern.<ref name="schaaf">{{cite book |author=Schaaf, Fred |date=2008 |title=The Brightest Stars |chapter=Appendix C |page=257 |publisher=Wiley |location=Hoboken, New Jersey |isbn=0-471-70410-5}}</ref> In the ], Rigel is the first bright star of Orion visible as the constellation rises.<ref>{{cite book|author=Ellyard, David|author2=Tirion, Wil |date=2008 |title=The Southern Sky Guide|edition = 3rd|origyear=1993|pages=58–59 |publisher=Cambridge University Press |location=Port Melbourne, Victoria |isbn= 978-0-521-71405-1}}</ref> | |||
| In ], Rigel is one of the most important ], since it is bright, easily located and equatorial, which means it is visible all around the world's oceans (the exception, areas within 8° of the North Pole). | |||
| ===Parallax=== | |||
| The new ] reduction of Rigel's parallax gives a distance of {{convert|863|ly|pc|abbr=off}}, with a ] of about 9%.<ref name=aaa474_2_653/> Earlier ] estimates placed its distance between {{convert|360|and|500|pc|ly|lk=on|abbr=off}}.<ref name=humphreys>{{cite journal|bibcode=1978ApJS...38..309H|title=Studies of luminous stars in nearby galaxies. I. Supergiants and O stars in the Milky Way|journal=Astrophysical Journal|volume=38|pages=309|author1=Humphreys|first1=R. M.|year=1978|doi=10.1086/190559}}</ref><ref name=bsc>{{cite journal |bibcode=1991bsc..book.....H |title=The Bright star catalogue |journal=New Haven |author1=Hoffleit |first1=Dorrit |last2=Jaschek |first2=Carlos |year=1991}}<</ref> | |||
| == System == | |||
| Rigel has been known as a ] since at least 1822, when it was measured by ].<ref name="WDS">{{cite web|url=http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/WDS|title=Washington Double Star Catalogue|work=US Naval Observatory|accessdate=13 March 2016}}</ref> Although the companion is not particularly faint at magnitude 6.7, with the separation of 9.5 arcsec in position angle 202° (2014), both components are resolvable in most amateur astronomer's telescopes.<ref name=WDS/> Its the large difference in brightness makes it a challenging target for telescope apertures smaller than {{convert|15.0|cm|in|abbr=on}}.<ref name="Burnham1978">{{cite book |title=Burnham's Celestial Handbook |last=Burnham |first=Robert, Jr. |date=1978 |publisher=Dover Publications |location=New York |page=1300 }}</ref> At Rigel's estimated distance, Rigel B's projected separation from its primary by over 2200 ]; Since discovery, there has been no sign of orbital movement, though both stars share similar ].<ref name="WDS"/><ref name="Jedicke1992">{{cite book |chapter=Regal Rigel |title=The New Cosmos |last=Jedicke |first=Peter |author2=Levy, David H. |date=1992 |publisher=Kalmbach Books |location=Waukesha |pages=48–53 }}</ref> The pair would have an minimum orbital period of around 18,000 years.<ref name=msc>{{cite journal|bibcode= 1997A&AS..124...75T|title= MSC - a catalogue of physical multiple stars|journal= A & A Supplement series|volume= 124|pages= 75|author1= Tokovinin|first1= A. A.|year= 1997|doi= 10.1051/aas:1997181}}</ref> | |||
| At various times since the 19th century, Rigel B has been reported to be resolved into a close binary of two equal components, with the measured separation varying from less than 0.1" to nearly 0.2". Speckle interferometry showed in 2009 two almost identical components separated by 0.124".<ref name=mason>{{cite journal|bibcode= 2009AJ....137.3358M|title= The High Angular Resolution Multiplicity of Massive Stars|journal= The Astronomical Journal|volume= 137|issue= 2|pages= 3358|author1= Mason|first1= Brian D.|last2= Hartkopf|first2= William I.|last3= Gies|first3= Douglas R.|last4= Henry|first4= Todd J.|last5= Helsel|first5= John W.|year= 2009|doi= 10.1088/0004-6256/137/2/3358}}</ref> Both stars would have apparent visual magnitudes of 7.6 with a likely orbital period of 63 years.<ref name=msc/> | |||
| Rigel B is itself a ] system, consisting of two ] stars that orbit each other every 9.86 days. The stars both belong to the spectral class B9. These two stars do not appear to make up the visual binary components B and C, so the system might be a triple star, although the true arrangement of them is unclear.<ref>{{cite web|url=http://sb9.astro.ulb.ac.be/ProcessMainform.cgi?Catalog=HD&Id=&Coord=05+14+32.2+-08+12+0+&Epoch=2000&radius=3&unit=arc+min|title=Spectroscopic Binary Catalogue (SB9)|work=D.Pourbaix|accessdate=13 March 2016}}</ref> | |||
| A 15.4 magnitude star at 44.6 arcsec in north position angle of 1° is catalogued as component D in the system although it is unclear whether it is physically related or a coincidental alignment.<ref name=WDS/> | |||
| == Properties == | |||
| ]]] | |||
| Moravveji and colleagues calculate a luminosity for Rigel A of 120,000 times that of the Sun.<ref name=apj2012_747_108/> Its surface temperature is around 12,100 K. The ]-measured ] of this star, after correction for ], is {{val|2.75|0.01|u=]}}.<ref name=auf/> At its estimated distance, this yields a size of about 79 times the ].<ref name=apj2012_747_108/> Przybilla and colleagues used atmospheric modelling in 2006 to come up with a distance of {{convert|360|±|40|pc|ly|abbr=off}}. They calculated it to be around 218,000 times as luminous as the Sun, and have around 21±3 ]es and 109±12 times its radius.<ref name=aaa445_3_1099/> The CMFGEN code is an atmosphere code used to determine the properties of massive stars from analysing their spectrum and atmosphere. Analysis of Rigel using this method yields a luminosity 279,000 times that of the Sun, a radius 115 times that of the Sun and stellar wind velocity of 671,080 miles per hour.<ref name="Chesneau 2014">{{cite journal|author=Chesneau, O.; Kaufer, A.; Stahl, O.; Colvinter, C.; Spang, A.; Dessart, L.; Prinja, R.; Chini, R.|date=2014|title=The variable stellar wind of Rigel probed at high spatial and spectral resolution|journal=Astronomy & Astrophysics|volume=566|id=A125 |pages=18|doi=10.1051/0004-6361/201322894 |bibcode=2014A&A...566A.125C|arxiv = 1405.0907 }}</ref> | |||
| Rigel A is a ] that has exhausted burning the hydrogen fuel in its core and left the main sequence, expanding and brightening as it progresses across the ]. Przybilla estimated that it has lost around 3 solar masses since beginning life as a star of 24 ± 3 solar masses 7 to 9 million years ago.<ref name=aaa445_3_1099/> It will become a red supergiant and eventually end its stellar life by exploding as a ], in the process flinging out material that will serve to seed future generations of stars.<ref name=apj2012_749_74/> It is one of the closest known potential supernova progenitors to Earth.<ref name=apj2012_747_108/> | |||
| Rigel's variability is complex and is caused by ] similar to those of ], the prototype of the class of ] pulsating stars. The radial velocity variations of Rigel proves that it simultaneously oscillates in at least 19 non-radial modes with periods ranging from about 1.2 to 74 days.<ref name=apj2012_747_108/> It is notable among blue supergiant stars in the sense that while its pulsations are powered by the nuclear reactions in a hydrogen-burning shell that is at least partially non-convective, the star also ] in its core.<ref name=apj2012_749_74 /> Rigel was identified as belonging to the Alpha Cygni variables in 1998 by Christoffel Waelkens and colleagues.<ref name="waelkens 1998">{{cite journal|author=Waelkens, C.; Aerts, C.; Kestens, E.; Grenon, M.; Eyer, L.|date=1998|title=Study of an unbiased sample of B stars observed with Hipparcos: the discovery of a large amount of new slowly pulsating B star|journal=Astronomy and Astrophysics|volume=330|pages=215–21|bibcode=1998A&A...330..215W}}</ref> | |||
| As it is both bright and moving through a region of nebulosity, Rigel lights up several dust clouds in its vicinity, most notably the ] (the Witch Head Nebula).<ref name="Jedicke1992">{{cite book |chapter=Regal Rigel |title=The New Cosmos |last=Jedicke |first=Peter |author2=Levy, David H. |date=1992 |publisher=Kalmbach Books |location=Waukesha |pages=48–53 }}</ref> Rigel is also associated with the ], which—while more or less along the same line of sight as the star—is almost twice as far away from Earth. Despite the difference in distance, projecting Rigel's path through space for its expected age brings it close to the nebula. As a result, Rigel is sometimes classified as an outlying member of the ] although it is considerably closer than most of the members. Betelgeuze and Saiph lie at a similar distance to Rigel, although Betelgeuze is a ] with a complex history and is likely to have originally formed in the main body of the association.<ref name=bally/> It has been listed as a member of the poorly-defined ]<ref name=racine>{{cite journal|bibcode=1968AJ.....73..233R|title=Stars in reflection nebulae|journal=Astronomical Journal Vol. 73|volume=73|pages=233|author1=Racine|first1=R.|year=1968|doi=10.1086/110624}}</ref> | |||
| The companions Rigel Ba, Bb, and C all appear to be similar B class main sequence stars of {{solar mass|3 - 4}}, but their properties are not accurately known.<ref name=msc/> | |||
| === Space photometry === | |||
| ] ] in ]. Rigel B is not visible in the glare of the main star.]] | |||
| Rigel was observed with the Canadian ] satellite for nearly 28 days in 2009. The light variations in this supergiant star were at the milli magnitude level. The gradual changes in the flux highlights the presence of long-period pulsation modes in the star.<ref name=apj2012_747_108/> | |||
| === Spectroscopy === | |||
| The general spectral type of Rigel as B8 is well-established and it has been used as a defining point of the spectral classification sequence for supergiants. However the details of the spectrum vary considerably owing to periodic atmospheric eruptions. The spectral lines show emission, absorption, line doubling, P Cygni profiles, and inverse P Cygni profiles, with no obvious periodicity.<ref name=rother>{{cite web|url= | |||
| http://rave.ohiolink.edu/etdc/view?acc_num=toledo1249043423|author=Rother, Sara|title=A time series study of Rigel, a B8Ia supergiant|date=2009}}</ref> This has resulted in classification as B8 Iab, B8 Iae, or blendings by different authors.<ref name=schultz>{{cite journal|bibcode=2014MNRAS.438.1114S|arxiv=1311.5116|title=An observational evaluation of magnetic confinement in the winds of BA supergiants|journal=Monthly Notices of the Royal Astronomical Society|volume=438|issue=2|pages=1114|author1=Shultz|first1=M.|last2=Wade|first2=G. A.|last3=Petit|first3=V.|last4=Grunhut|first4=J.|last5=Neiner|first5=C.|last6=Hanes|first6=D.|author7=MiMeS Collaboration|year=2014|doi=10.1093/mnras/stt2260}}</ref><ref name=bally>{{cite journal|bibcode=2008hsf1.book..459B|arxiv=0812.0046|title=Overview of the Orion Complex|journal=Handbook of Star Forming Regions|pages=459|author1=Bally|first1=J.|year=2008}}</ref> | |||
| == Names == | |||
| The modern name ''Rigel'' is first recorded in the ] of 1252. | |||
| It is derived from the Arabic name ''{{transl|ar|Rijl Jauzah al Yusrā}}'', "the left leg (foot) of Jauzah" (i.e. ''rijl'' meaning "leg, foot").<ref name="allen">{{cite book | |||
| | author=Allen, Richard Hinckley | |||
| | author-link=Richard Hinckley Allen | |||
| | date=1963 |origyear=1899 | |||
| | title=Star Names: Their Lore and Meaning | |||
| | edition=] | |||
| | publisher=] Inc. | |||
| | location=], ] | |||
| | url= http://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Orion*.html | |||
| | isbn=0-486-21079-0 | |||
| | pages = 312–13}}</ref> | |||
| The Arabic name can be traced to the 10th century.<ref name="KUNITZSCH1959">{{cite book | |||
| |author=Kunitzsch, Paul | |||
| |date=1959 | |||
| |title=Arabische Sternnamen in Europa | |||
| |publisher=] | |||
| |location=] | |||
| |page=46}}</ref> "Jauzah" was a proper name of the Orion figure, an alternative Arabic name was {{lang|ar|رجل الجبار}} ''{{transl|ar|riǧl al-ǧabbār}}'', "the foot of the great one", which is the source of the rarely used variant names ''Algebar'' or ''Elgebar''. The ''Alphonsine Tables'' saw its name split into "Rigel" and "Algebar", with the note, "et dicitur Algebar. Nominatur etiam Rigel."<ref name=Kunitzsch86>{{cite journal|bibcode = 1986JHA....17...89K|title = The Star Catalogue Commonly Appended to the Alfonsine Tables|journal = Journal for the History of Astronomy|volume = 17|pages = 89|author1 = Kunitzsch|first1 = P.|year = 1986}}</ref> | |||
| Alternate spellings from the 17th century include ''Regel'' by ], ''Riglon'' by ], and ''Rigel Algeuze'' or ''Algibbar'' by ].<ref name="allen"/> | |||
| <!-- | |||
| In ancient Egypt Rigel's name was <hiero>S29-Aa17-V28-D61-N14:N35</hiero>Seba-en-Sah ''{{Unicode|Sb3-n-S3ḥ}}'', which means ''toe star'' or ''foot star''.{{cn}} | |||
| --> | |||
| Rigel is presumably the star known as "]'s toe" in ].<ref>Richard Cleasby, ''An Icelandic-English Dictionary, Clarendon Press, 1874, s.v. ''auvandils-tá''.</ref> | |||
| In Chinese astronomy, Rigel is the seventh star of the "]" asterism, {{lang|zh|参宿七}} (''{{lang|zh-Latn|Shēnxiù Qī}}''). | |||
| In Japan, the Minamoto or ] had chosen Rigel and its white color as its symbol, calling the star ''Genji-boshi'' ({{lang|ja|源氏星}}), while the Taira or ] adopted Betelgeuse and its red color. The two powerful families fought a ] in Japanese history, the stars seen as facing each other off and only kept apart by the Belt.<ref name="RENSHAW1">{{cite web | |||
| |title=Yowatashi Boshi; Stars that Pass in the Night | |||
| |author=Steve Renshaw | |||
| |author2=Saori Ihara | |||
| |last-author-amp=yes | |||
| |publisher=Griffith Observer | |||
| |url=http://www2.gol.com/users/stever/orion.htm | |||
| |date=October 1999 | |||
| |accessdate=25 June 2012}}</ref><ref>"]" p. 815 ISBN 978-4-385-13902-9</ref><ref>] "Shin seiza jyunrei" p. 19 ISBN 978-4-12-204128-8</ref> Rigel was also known as ''Gin-waki'', ({{lang|ja|銀脇}}), "the Silver (Star) beside ('']'')." | |||
| <!-- | |||
| In India, Rigel is known as ''Mrugasheersha'', meaning 'Deer's Head'. In the ], it is known as ''Vaan Raja''.{{cn}} | |||
| --> | |||
| Rigel was known as ''Yerrerdet-kurrk'' to the Wotjobaluk ] of southeastern Australia, and held to be the mother-in-law of ''Totyerguil'' (]). The distance between them signified the taboo preventing a man from approaching his mother-in-law.<ref>{{cite book|last=Mudrooroo|title=Aboriginal mythology : an A-Z spanning the history of aboriginal mythology from the earliest legends to the present day|publisher=HarperCollins|location=London|date=1994|page=142|isbn=978-1-85538-306-7}}</ref> | |||
| The indigenous ] people of northwestern Victoria named Rigel as ''Collowgullouric Warepil''.<ref name=hamacher>{{cite journal|author=Hamacher, Duane W.|author2=Frew, David J. |date=2010|title= An Aboriginal Australian Record of the Great Eruption of Eta Carinae|journal=Journal of Astronomical History & Heritage |volume=13|issue=3|pages= 220–34|bibcode=2010JAHH...13..220H |arxiv = 1010.4610 }}</ref> | |||
| The ] of northern Australia know Rigel as the Red Kangaroo Leader ''Unumburrgu'' and chief conductor of ceremonies in a songline when Orion is high in the sky. The river Eridanus marks a line of stars in the sky leading to it, and the other stars of Orion are his ceremonial tools and entourage. Betelgeuse is ''Ya-jungin'' "Owl Eyes Flicking", watching the ceremonies.<ref>{{cite book | last1 = Harney | first1 = Bill Yidumduma | last2 = Cairns | first2 = Hugh C. | title = Dark Sparklers | publisher = Hugh C. Cairns | location = Merimbula, New South Wales |pages=139–40 | date = 2004 | origyear = 2003 | edition = Revised | isbn = 0-9750908-0-1}}</ref> | |||
| The ] named Rigel as '']'' and was said to be a daughter of ''Rehua'' (]), the chief of all stars.<ref>p. 419, , Janet Parker, Alice Mills, Julie Stanton, Durban, Struik Publishers, 2007.</ref> Its heliacal rising also presaged the appearance of '']'' (the ]) in the dawn sky which marked the Māori New Year in late May or early June. The ] of the Chatham Islands, as well as some Maori groups in New Zealand marked the start of their New Year with Rigel rather than the Pleiades.<ref name="kelley">{{cite book|author=Kelley, David H.|author2=Milone, Eugene F. |title=Exploring Ancient Skies: A Survey of Ancient and Cultural Astronomy|publisher=Springer|date=2011|page=341|isbn=144197623X|url=https://books.google.com/?id=ILBuYcGASxcC&pg=PA341&lpg=PA341&dq=Puanga+Rigel#v=onepage&q=Puanga%20Rigel&f=false}}</ref> ''Puaka'' was a local variant used in the South Island.<ref name="Best22">{{cite book|last=Best|first=Elsdon|title=Astronomical Knowledge of the Maori: Genuine and Empirical|publisher=Dominion Museum|location=Wellington, New Zealand|date=1922|pages=39–40|url=http://nzetc.victoria.ac.nz/tm/scholarly/tei-BesAstro-t1-body-d1-d6-d4.html}}</ref> | |||
| The ] knew it as ''tunsel'' "little woodpecker".<ref>{{cite book|last=Milbrath|first=Susan |title=Star Gods of the Maya: Astronomy in Art, Folklore, and Calendars|publisher=University of Texas Press|location=Austin, Texas|date=1999|page=39|isbn=0292752261|url=https://books.google.com/?id=DgqLplWtGPgC&pg=PA39&dq=betelgeuse+folklore#v=onepage&q=betelgeuse%20folklore&f=false}}</ref> | |||
| == See also == | |||
| {{Portal|Astronomy|Star}} | |||
| * ] | |||
| {{clear}} | |||
| == References == | |||
| {{Reflist|30em|refs= | |||
| <ref name=aaa474_2_653>{{cite journal | 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=aass34_1>{{cite journal | last1=Nicolet | first1=B. | date=1978 | title=Photoelectric photometric Catalogue of homogeneous measurements in the UBV System | journal=Astronomy and Astrophysics Supplement Series | volume=34 | pages=1–49 | bibcode=1978A&AS...34....1N }}</ref> | |||
| <ref name=aaa445_3_1099>{{cite journal | display-authors=1 | last1=Przybilla | first1=N. | last2=Butler | first2=K. | last3=Becker | first3=S. R. | last4=Kudritzki | first4=R. P. | title=Quantitative spectroscopy of BA-type supergiants | journal=Astronomy and Astrophysics | volume=445 | issue=3 | pages=1099–1126 |date=January 2006 | doi=10.1051/0004-6361:20053832 | bibcode=2006A&A...445.1099P |arxiv = astro-ph/0509669 }}</ref> | |||
| <ref name="simbad">{{cite web | title=SIMBAD Astronomical Database | work=Results for Rigel | url=http://simbad.u-strasbg.fr/Simbad | accessdate=2008-04-10 }}</ref> | |||
| <ref name=baas25_1319>{{cite journal | last1=Garrison | first1=R. F. | title=Anchor Points for the MK System of Spectral Classification | journal=Bulletin of the American Astronomical Society | volume=25 | page=1319 |date=December 1993 | bibcode=1993AAS...183.1710G}}</ref> | |||
| <ref name=apj2012_747_108>{{cite journal | last1=Moravveji | first1=Ehsan | last2=Guinan | first2=Edward F. | last3=Shultz | first3=Matt | last4=Williamson | first4=Michael H. | last5=Moya | first5=Andres | title=Asteroseismology of the nearby SN-II Progenitor: Rigel. Part I. The ''MOST'' High-precision Photometry and Radial Velocity Monitoring | journal=The Astrophysical Journal | volume=747 | issue=1 | pages=108–115 |date=March 2012 | doi=10.1088/0004-637X/747/2/108 | bibcode=2012ApJ...747..108M |arxiv = 1201.0843 }}</ref> | |||
| <ref name=apj2012_749_74>{{cite journal | last1=Moravveji | first1=Ehsan | last2=Moya | first2=Andres | last3=Guinan | first3=Edward F. | title=Asteroseismology of the nearby SN-II Progenitor: Rigel. Part II. ε-mechanism Triggering Gravity-mode Pulsations? | journal=The Astrophysical Journal | volume=749 | issue=1 | pages=74–84 |date=April 2012 | doi=10.1088/0004-637X/749/1/74 | bibcode=2012ApJ...749..74M }}</ref> | |||
| <ref name=auf>{{cite journal | last1=Aufdenberg | first1=J. P. | title=Limb Darkening: Getting Warmer | journal=The Power of Optical/IR Interferometry | volume=1 | issue=1 | pages=71–82 | date=2008 | doi=10.1007/978-3-540-74256-2_8 | bibcode=2008poii.conf...71A |display-authors=etal| series=Eso Astrophysics Symposia | isbn=978-3-540-74253-1 }}</ref> | |||
| }} | |||
| == External links == | |||
| {{Commonscat-inline|Rigel}} | |||
| * from ] | |||
| {{Stars of Orion}} | |||
| {{Sky|05|14|32.272|-|08|12|05.91|800}} | |||
| ] | |||
| ] | |||
| ] | |||
| ] | |||
| ] | |||
| ] | |||
| ] | |||
| ] | |||
| ] | |||
| ] | |||
| ] | |||
| ] | |||
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