فم الحوت

هذا المقال هو عن the star. إذا كنت تريد the extrasolar planet، انظر Fomalhaut b.


Fomalhaut
Heic0821f.jpg
DSS image of Fomalhaut, field of view 2.7×2.9 degrees.
Credit NASA, ESA, and the Digitized Sky Survey 2. Acknowledgment: Davide De Martin (ESA/Hubble)
بيانات الرصـد
Epoch J2000      Equinox J2000
Constellation Piscis Austrinus, Aquarius
Fomalhaut
Right ascension 22h 57m 39.0465s[1]
Declination −29° 37′ 20.050″[1]
Apparent magnitude (V) 1.16
TW Piscis Austrini
Right ascension 22h 56m 24.05327s[1]
Declination −31° 33′ 56.0351″[1]
Apparent magnitude (V) 6.48[2]
LP 876-10
Right ascension 22h 48m 04.47s[3]
Declination -24° 22′ 07.5″[3]
Apparent magnitude (V) 12.618[3]
الخـصـائص
النوع الطيفيA3 V / K5Vp / M4V[4][3]
U-B دليل الألوان0.08 / 1.02 / ?[5]
B-V دليل الألوان0.09 / 1.10 / 1.683[5][3]
النوع المتغيرNone / BY Draconis / ?
علم القياسات الفلكية
السرعة القطرية (Rv)+6.5 كم/ث
الحركة الحقيقية (μ) RA: +328.95[1] mas/yr
Dec.: −164.67[1] mas/س
اختلاف المنظر (π)129.81 ± 0.47[1] mas
المسافةس ض
( ف ن)
القدر المطلق (MV)1.72[6]
التـفـاصـيل
Fomalhaut
الكتلة1.92±0.02[6] M☉
نصف القطر1.842±0.019[6] R☉
جاذبية السطح (log g)4.21[7]
الضياء16.63±0.48[6] L☉
درجة الحرارة8,590[6] ك
سرعة الدوران (v sin i)93[7] كم/ث
العمر(4.4±0.4)×108[6] سنة
TW Piscis Austrini
الكتلة0.725 ± 0.036[4] M☉
نصف القطر0.629 ± 0.051[4] R☉
الضياء0.19[6] L☉
Temperature4,711 ± 134[4] ك
سرعة الدوران (v sin i)2.93[4] كم/ث
العمر4.4 × 108[6] سنة
تسميات أخرى
مراجع قواعد البيانات
SIMBADdata
ARICNSdata
Extrasolar Planets
Encyclopaedia		data
مراجع قواعد البيانات
SIMBADdata
ARICNSdata

فم الحوت نجم يقع في كوكبة الحوت الجنوبي يبعد حوالي 25 سنة ضوئية (7,688 فرسخ فلكي)عن الأرض، تبلغ حرارته 5800 كلفن. ويعتبر هذا النجم واحداً من النجوم العشرين التي تتربع على عرش البريق في السماء لونه ضارب إلى الزرقة وظهوره يعلن بداية فصل الخريف. يعتقد أن فم الحوت يصدر أشعة تحت الحمراء.

Fomalhaut (Alpha Piscis Austrini, Alpha PsA, α Piscis Austrini, α PsA) is the brightest star in the constellation Piscis Austrinus and one of the brightest stars in the sky. It is a class A star on the main sequence approximately 25 light-years (7.7 pc) from Earth as measured by the Hipparcos astrometry satellite.[8] Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.[9] It is classified as a Vega-like star that emits excess infrared radiation, indicating it is surrounded by a circumstellar disk.[10] Fomalhaut, K-type star TW Piscis Austrini and M-type star LP 876-10 constitute a trinary system.[11]

Fomalhaut holds a special significance in extrasolar planet research, as it is the center of the first stellar system with an extrasolar planet candidate (Fomalhaut b) imaged at visible wavelengths. The image was published in Science in November 2008.[12] Fomalhaut is the third brightest star known to have a planetary system, after Pollux and the Sun.


فم الحوت

. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

المعلومات

فم الحوت نجم يقع في كوكبة الحوت الجنوبي يبعد حوالي 25 سنة ضوئية (7,688 فرسخ فلكي)عن الأرض، تبلغ حرارته 5800 كلفن. ويعتبر هذا النجم واحداً من النجوم العشرين التي تتربع على عرش البريق في السماء لونه ضارب إلى الزرقة وظهوره يعلن بداية فصل الخريف. يعتقد أن فم الحوت يصدر أشعة تحت الحمراء.

فهو نجم يحمل أهمية خاصة في مجال البحوث خارج المجموعة الشمسية. لأنها مركز النظام النجمي الأول خارج المجموعة الشمسية لتصوير الموجات المرئية. وقد نشرت هذه الصورة للعلم في نوفمبر 2008. وهو ثالث نجم لامع يدور حول كوكب مع النجمين (بولكس Pollux) والشمس. ومن المعتقد أن نجم (فم الحوت Fomalhaut) هو نجم شاب، فقط عمره من 100 : 300 مليون سنة، ودرجة حرارة سطح هذا النجم حوالي 8751 كيلفن (8478 درجة مئوية). كتلة هذا النجم حوالي 2.1 مرة من كتلة الشمس ولها لمعان حوالي 18 ضعف. وقطرها حوالي 1.8 أكبـر. و هو من النجوم ناقصة المعادن بالنسبة للشمس وهو ما يعني أنها تتكون من كميات ونسب أقل من الهيدروجين والهليوم.

وهو أحد النجوم الـ 16 الذين ينتمون إلى (مجموعة نقل كاستورCastor Moving Group) المتحركة، وهذه المجموعة هي رابطة للنجوم التي تحلق بالفضاء مشتركةً مع بعضها البعض. وبالتالي فإنه من المرجح أن تكون مرتبطة فعلياً، ويحيط بالنجم (فم الحوت Fomalhaut) قرص محطم من الغبار في شكل حلقي مع حافة داخلية حادة جداً، وهو يميل ب 24 درجة من على الحافة. ويوزع الغبار بمسافة 25 وحدة فلكية ,ومن المعروف أن كمية الأشعة الحمراء المنبعثة منه كبيرة. في 13 نوفمبر 2008 أعلن علماء الفلك اكتشاف كوكب خارج المجموعة الشمسية، وكان هذا أول كوكب يُنظر إليه خارج المجموعة الشمسية بسبب تلسكوب الفضاء هبل. وكان وجود الكوكب يشتبه به في السابق.


نظام Fomalhaut C [13]
المرافق
(بالترتيب من النجم) 		الكتلة نصف المحور الرئيسي
(و.ف.) 		الدور المداري
(يوم) 		الانحراف الميل نصف القطر
Debris disk ~10–<40 AU — —

ومن الظاهر أن اسم [ Fomalhaut ] مأخوذ من الاسم العربي [ فم الحوت ]. في میل 29.6°-يقع [ فم الحوت ] في جنوب خط الإستواء السماوي وبالتالي يتم عرضه بشكل أفضل من نصف الكرة الأرضية الجنوبي وهو يمر فعلياً من مدار الحمل إلى الجنوب [ مدار الجدي ]. ويُرى على سبيل المثال من [ Brisbane, Johannesburg and Easter Island بريسبان وجوهانسبرغ وجزيرة الفصح].. ولكن الإنحراف في الجنوب ليس كبيراً بشكل كبير مثل النجوم الآتية : [ Acrux, Alpha Centauri and Canopus, أكراكس، الفا قنطورس وكانوب ]


Fomalhaut A

Dust ring around Fomalhaut from the Atacama Large Millimeter/submillimeter Array (ALMA)[14]

At a declination of −29.6°, Fomalhaut is located south of the celestial equator, and hence is best viewed from the Southern Hemisphere. However, its southerly declination is not as great as that of stars such as Acrux, Alpha Centauri and Canopus, meaning that, unlike them, Fomalhaut is visible from a large part of the Northern Hemisphere as well. Its declination is greater than that of Sirius and similar to that of Antares. At 40°N, Fomalhaut rises above the horizon for eight hours and reaches only 20° above the horizon, while Capella which rises at approximately the same time will stay above the horizon for twenty hours. From إنگلترة the star never appears much brighter than magnitude 2.2 due to it being so close to the horizon, and from southern Alaska or Scandinavia it never rises above the horizon at all.[15] Fomalhaut can be located in these northern latitudes by the fact that the western (right-hand) side of the Square of Pegasus points to it. Continue the line from Beta to Alpha Pegasi towards the southern horizon: Fomalhaut is about 45˚ south of Alpha Pegasi, with no bright stars in between.[16]

الخصائص

The debris disk around the star

Fomalhaut is a young star, for many years thought to be only 100 to 300 million years old, with a potential lifespan of a billion years.[17][18] A 2012 study gave a slightly higher age of 440±40 million years.[6] The surface temperature of the star is around 8,590 K (8,320 °C). Fomalhaut's mass is about 1.92 times that of the Sun, its luminosity is about 16.6 times greater, and its diameter is roughly 1.84 times as large.[6]

Fomalhaut is slightly metal-deficient as compared to the Sun, which means it is composed of a smaller percentage of elements other than hydrogen and helium.[7] The metallicity is typically determined by measuring the abundance of iron in the photosphere relative to the abundance of hydrogen. A 1997 spectroscopic study measured a value equal to 93% of the Sun's abundance of iron.[19][nb 1] A second 1997 study deduced a value of 78% by assuming Fomalhaut has the same metallicity as the neighboring star TW Piscis Austrini, which has since been argued to be a physical companion.[6][20] In 2004, a stellar evolutionary model of Fomalhaut yielded a metallicity of 79%.[7] Finally, in 2008, a spectroscopic measurement gave a significantly lower value of 46%.[21]

Fomalhaut has been claimed to be one of approximately 16 stars belonging to the Castor Moving Group. This is an association of stars that share a common motion through space and have been claimed to be physically associated. Other members of this group include Castor and Vega. The moving group has an estimated age of 200±100 million years and originated from the same location.[17] Unfortunately more recent work that has found that purported members of the Castor Moving Group appear to not only have a wide range of ages, but their velocities are too different to have been possibly associated with one another in the distant past.[11] Hence, "membership" to this dynamical group has no bearing on the age of the Fomalhaut system.[11]

أقراص الركام والكوكب

Debris ring around Fomalhaut showing location of planet Fomalhaut b—imaged by
Hubble Space Telescope's coronagraph.
(January 8, 2013) (NASA).

Fomalhaut is surrounded by several debris disks.

The inner disk is a high-carbon small-grain (10-300 nm) ash disk clustering at 0.1 AU from the star. Next is a disk of larger particles with inner edge 0.4-1 AU of the star. The innermost disk is unexplained as yet.[10]

The outermost disk is at a radial distance of 133 AU (1.99×1010 km; 1.24×1010 mi), in a toroidal shape with a very sharp inner edge, all inclined 24 degrees from edge-on.[22][23] The dust is distributed in a belt about 25 AU wide. The geometric center of the disk is offset by about 15 AU (2.2×109 km; 1.4×109 mi) from Fomalhaut.[24] The disk is sometimes referred to as "Fomalhaut's Kuiper belt". Fomalhaut's dusty disk is believed to be protoplanetary,[25] and emits considerable infrared radiation. Measurements of Fomalhaut's rotation indicate that the disk is located in the star's equatorial plane, as expected from theories of star and planet formation.[26]

On November 13, 2008, astronomers announced an object, which they assumed to be an extrasolar planet, orbiting just inside the outer debris ring. This was the first extrasolar orbiting object to be seen with visible light, captured by the Hubble Space Telescope.[27] A planet's existence had been previously suspected from the sharp, elliptical inner edge of that disk.[28] The mass of the planet, Fomalhaut b, was estimated to be no more than three times the mass of Jupiter but at least the mass of Neptune.[29] There are indications that the orbit is not apsidally aligned with the dust disk, which may indicate that additional planets may be responsible for the dust disk's structure.[30]

However M-band images taken from the MMT Observatory put strong limits on the existence of gas giants within 40 AU of the star[31] and Spitzer Space Telescope imaging suggested that the object Fomalhaut b was more likely to be a dust cloud.[32] In 2012, two independent studies confirmed that Fomalhaut b does exist; but it is shrouded by debris, so it may be a gravitationally-bound accumulation of rubble rather than a whole planet.[33][34]

Herschel Space Observatory images of Fomalhaut reveal a large amount of fluffy micrometer-sized dust is present in the outer dust belt. Because such dust is expected to be blown out of the system by stellar radiation pressure on short timescales, its presence indicates a constant replenishment by collisions of planetesimals. The fluffy morphology of the grains suggests a cometary origin. The collision rate is estimated to be approximately 2000 kilometre-sized comets per day.[35]

Observations of the star's outer dust ring by the Atacama Large Millimeter Array point to the existence of two planets in the system, neither one at the orbital radius proposed for the HST-discovered Fomalhaut b.[36]

If there are additional planets from 4 to 10 AU, they must be under 20 MJ; if from 2.5 outward, then 30 MJ.[37]


نظام فم الحوت [10][38]
المرافق
(بالترتيب من النجم) 		الكتلة نصف المحور الرئيسي
(و.ف.) 		الدور المداري
(سنة) 		الانحراف الميل نصف القطر
القرص الساخن الداخلي 0.08–0.11 AU — —
القرص الساخن الخارجي 0.21–0.62 و.ف. أو 0.88–1.08 و.ف. — —
حزام 10 و.ف. 8–12 AU — —
قرص الغبار بين الأحزمة 35–133 AU — —
ب ؟ MJ 177±68 ~1700 0.8±0.1 —
الحزام الرئيسي 133–158 AU −66.1° —
الهالة الخارجية للحزام الرئيسي 158–209 AU — —

انظر أيضا

الهامش

  1. ^ Calculation of metallicity: if m = [Fe/H], then the ratio of iron to hydrogen for Fomalhaut divided by the ratio of iron to hydrogen for the Sun is given by 10m.

الهامش

  1. ^ أ ب ت ث ج ح خ van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357{{cite journal}}: CS1 maint: postscript (link)
  2. ^ "V* TW PsA -- Variable of BY Dra type". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-01-20.
  3. ^ أ ب ت ث ج "LP 876-10 -- Double or multiple star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2014-07-30.
  4. ^ أ ب ت ث ج Demory, B.-O.; Ségransan, D.; Forveille, T.; Queloz, D.; Beuzit, J.-L.; Delfosse, X.; di Folco, E.; Kervella, P.; et al. (October 2009), "Mass-radius relation of low and very low-mass stars revisited with the VLTI", Astronomy and Astrophysics 505 (1): 205–215, doi:10.1051/0004-6361/200911976, Bibcode: 2009A&A...505..205D 
  5. ^ أ ب Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99). Bibcode:1966CoLPL...4...99J.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  6. ^ أ ب ت ث ج ح خ د ذ ر ز Mamajek, E.E. (August 2012). "On the Age and Binarity of Fomalhaut". Astrophysical Journal Letters. 754 (2): L20. arXiv:1206.6353. Bibcode:2012ApJL..754...20M. doi:10.1088/2041-8205/754/2/L20.
  7. ^ أ ب ت ث Di Folco, E.; Thévenin, F.; Kervella, P.; Domiciano de Souza, A.; Coudé du Foresto, V.; Ségransan, D.; Morel, P. (November 2004). "VLTI near-IR interferometric observations of Vega-like stars. Radius and age of α PsA, β Leo, β Pic, ɛ Eri and τ Cet". Astronomy and Astrophysics. 426 (2): 601–617. Bibcode:2004A&A...426..601D. doi:10.1051/0004-6361:20047189.{{cite journal}}: CS1 maint: multiple names: authors list (link) This paper lists [Fe/H] = −0.10 dex.
  8. ^ Perryman, Michael (2010), The Making of History's Greatest Star Map, Heidelberg: Springer-Verlag, doi:10.1007/978-3-642-11602-5 
  9. ^ Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society 25: 1319, Bibcode: 1993AAS...183.1710G, http://www.astro.utoronto.ca/~garrison/mkstds.html, retrieved on 2012-02-04 
  10. ^ أ ب ت B. Mennesson, O. Absil, J. Lebreton, J.-C. Augereau, E. Serabyn, M. M. Colavita, R. Millan-Gabet, W. Liu, P.Hinz, P. Thebault (2012), "An interferometric study of the Fomalhaut inner debris disk II. Keck Nuller mid-infrared observations", Astrophysical Journal, doi:10.1088/0004-637X/763/2/119, Bibcode: 2013ApJ...763..119M 
  11. ^ أ ب ت DOI:10.1088.2F0004-6256.2F146.2F6.2F154
    This citation will be automatically completed in the next few minutes. You can jump the queue or expand by hand
  12. ^ Kalas, Paul; et al. (2008). "Optical Images of an Exosolar Planet 25 Light-Years from Earth". Science. 322 (5906): 1345–1348. arXiv:0811.1994. Bibcode:2008Sci...322.1345K. doi:10.1126/science.1166609. PMID 19008414. {{cite journal}}: Explicit use of et al. in: |author2= (help)
  13. ^ Kennedy, Grant M.; et al. (2013-12-17). "Discovery of the Fomalhaut C debris disc". Monthly Notices of the Royal Astronomical Society. arXiv:1312.5315. Bibcode:2013arXiv1312.5315K. doi:10.1093/mnrasl/slt168.
  14. ^ "ALMA Reveals Workings of Nearby Planetary System". ESO Press Release. Retrieved 13 April 2012.
  15. ^ Fred Schaaf (2008). The Brightest Stars: Discovering the Universe through the Sky's Most Brilliant Stars. John Wiley & Sons. p. 231. ISBN 047024917X.
  16. ^ "Shallow Sky Object of the Month: Fomalhaut". Houston Astronomical Society. August 2013. Retrieved 2014-07-30.
  17. ^ أ ب Barrado y Navascues, D. (1998). "The Castor moving group. The age of Fomalhaut and VEGA". Astronomy and Astrophysics. 339: 831–839. arXiv:astro-ph/9905243. Bibcode:1998A&A...339..831B.
  18. ^ "Elusive Planet Reshapes a Ring Around Neighboring Star". HubbleSite - newscenter. Space Telescope Science Institute (STScI). June 22, 2005.
  19. ^ Dunkin, S. K.; Barlow, M. J.; Ryan, Sean G.; Barlow; Ryan (April 1997). "High-resolution spectroscopy of Vega-like stars - I. Effective temperatures, gravities and photospheric abundances". Monthly Notices of the Royal Astronomical Society. 286 (3): 604–616. Bibcode:1997MNRAS.286..604D. doi:10.1093/mnras/286.3.604.{{cite journal}}: CS1 maint: multiple names: authors list (link) This paper lists [Fe/H] = −0.03 dex.
  20. ^ Barrado y Navascues, David; Stauffer, John R.; Hartmann, Lee; Balachandran, Suchitra C. (January 1997). "The Age of Gliese 879 and Fomalhaut". Astrophysical Journal. 475: 313. arXiv:astro-ph/9704021. Bibcode:1997ApJ...475..313B. doi:10.1086/303518.{{cite journal}}: CS1 maint: multiple names: authors list (link) This paper lists [Fe/H] = −0.11 dex.
  21. ^ Saffe, C.; Gómez, M.; Pintado, O.; González, E. (October 2008). "Spectroscopic metallicities of Vega-like stars". Astronomy and Astrophysics. 490 (1): 297–305. arXiv:0805.3936. Bibcode:2008A&A...490..297S. doi:10.1051/0004-6361:200810260.{{cite journal}}: CS1 maint: multiple names: authors list (link) This paper lists [Fe/H] = −0.34 dex.
  22. ^ Kalas, Paul; Graham, James R.; Clampin, Mark (2005). "A planetary system as the origin of structure in Fomalhaut's dust belt". Nature. 435 (7045): 1067–1070. arXiv:astro-ph/0506574. Bibcode:2005Natur.435.1067K. doi:10.1038/nature03601. PMID 15973402.
  23. ^ The disc was reported by Holland, Wayne S.; et al. (1998). "Submillimetre images of dusty debris around nearby stars". Nature. 392 (6678): 788–791. Bibcode:1998Natur.392..788H. doi:10.1038/33874. {{cite journal}}: Explicit use of et al. in: |author2= (help) They noted that the disc was centered on a cavity, which they suggested might have been swept out by planets.
  24. ^ "Fomalhaut's Kuiper Belt". Sky & Telescope. Retrieved October 16, 2007.
  25. ^ "Hubble Directly Observes a Planet Orbiting Another Star". Retrieved November 13, 2008.
  26. ^ Le Bouquin, Jean-Baptiste; et al. (2009). "The spin-orbit alignment of the Fomalhaut planetary system probed by optical long baseline interferometry". arXiv:0904.1688. {{cite arXiv}}: Explicit use of et al. in: |author= (help); Unknown parameter |type= ignored (help)
  27. ^ "From afar, the first optical photos of an exoplanet". AFP. 2008-11-13.
  28. ^ Predictions for a planet just inside Fomalhaut's eccentric ring, Alice C. Quillen, Monthly Notices of the Royal Astronomical Society, 372, #1 (October 2006), pp. L14–L18, DOI:10.1111/j.1745-3933.2006.00216.x, قالب:Bibcode.
  29. ^ Paul Kalas (2008-11-13). "Direct Image Of Extrasolar Planet". Retrieved 2008-11-14. (at 3 minutes 45 seconds: "... has to be less than three Jupiter masses. In fact our lower limit to Fomalhaut b is Neptune")
  30. ^ Chiang, E.; et al. (2008). "Fomalhaut's Debris Disk and Planet: Constraining the Mass of Fomalhaut b From Disk Morphology". arXiv:0811.1985. {{cite arXiv}}: Explicit use of et al. in: |author= (help); Unknown parameter |type= ignored (help); Unknown parameter |version= ignored (help)
  31. ^ Kenworthy, Matthew A.; et al. (2008). "MMT/AO 5 micron Imaging Constraints on the Existence of Giant Planets Orbiting Fomalhaut at ~13-40 AU". arXiv:0811.2443. {{cite arXiv}}: Explicit use of et al. in: |author= (help); Unknown parameter |type= ignored (help); Unknown parameter |version= ignored (help)
  32. ^ Markus, J.; et al. (2012). "Infrared Non-detection of Fomalhaut b—Implications for the Planet Interpretation". arXiv:1201.4388. {{cite arXiv}}: Explicit use of et al. in: |author= (help); Unknown parameter |type= ignored (help); Unknown parameter |version= ignored (help)
  33. ^ Raphael Galicher, Christian Marois, B. Zuckerman, Bruce Macintosh. "Fomalhaut b: Independent Analysis of the Hubble Space Telescope Public Archive Data". The Astrophysical Journal. arXiv:1210.6745. Bibcode:2013ApJ...769...42G. doi:10.1088/0004-637X/769/1/42.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  34. ^ Thayne Currie; et al. "Direct Imaging Confirmation and Characterization of a Dust-Enshrouded Candidate Exoplanet Orbiting Fomalhaut". The Astrophysical Journal Letters. arXiv:1210.6620. Bibcode:2012ApJ...760L..32C. doi:10.1088/2041-8205/760/2/L32. {{cite journal}}: Explicit use of et al. in: |author= (help)
  35. ^ "Herschel images of Fomalhaut. An extrasolar Kuiper belt at the height of its dynamical activity". Astronomy & Astrophysics (class: astro-ph). 2012. arXiv:1204.5037. Bibcode:2012A&A...540A.125A. doi:10.1051/0004-6361/201118581. {{cite journal}}: Cite uses deprecated parameter |authors= (help)
  36. ^ Boley, A.; et al. (2012). "Constraining the Planetary System of Fomalhaut Using High-Resolution ALMA Observations". arXiv:1204.0007. {{cite arXiv}}: Explicit use of et al. in: |author= (help); Unknown parameter |type= ignored (help); Unknown parameter |version= ignored (help)
  37. ^ "Coronagraphic Observations of Fomalhaut at Solar System Scales". Astrophysical Journal (class: astro-ph). 2012. arXiv:1212.1459. Bibcode:2013ApJ...764....7K. doi:10.1088/0004-637X/764/1/7. {{cite journal}}: Cite uses deprecated parameter |authors= (help)
  38. ^ Kalas, Paul; Graham, James R.; Fitzgerald, Michael P.; Clampin, Mark (2013). "STIS Coronagraphic Imaging of Fomalhaut: Main Belt Structure and the Orbit of Fomalhaut b". The Astrophysical Journal. 775 (1): article id. 56. arXiv:1305.2222. Bibcode:2013ApJ...775...56K. doi:10.1088/0004-637X/775/1/56.{{cite journal}}: CS1 maint: multiple names: authors list (link)


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وصلات خارجية

الإحداثيات: خريطة السماء 22س 57ق 39.1ث, −29° 37′ 20″

قالب:Stars of Piscis Austrinus

الكلمات الدالة:
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