القفزة الثالثة الشمالية

(تم التحويل من Iota Ursae Majoris)
Iota Ursae Majoris
Diagram showing star positions and boundaries of the Ursa Major constellation and its surroundings
Diagram showing star positions and boundaries of the Ursa Major constellation and its surroundings

Location of ι Ursae Majoris (circled)
بيانات الرصـد
الحقبة J2000      اعتدال J2000
الكوكبة Ursa Major
الصعود المستقيم 08h 59m 12.45362s[1]
الميل +48° 02′ 30.5741″[1]
القدر الظاهري (V)3.14[2]/10.1/10.3
الخـصـائص
النوع الطيفيA7V(n)[3] + M3V + M4V[4]
U-B دليل الألوان+0.08[2]
B-V دليل الألوان+0.19[2]
النوع المتغيرSuspected
علم القياسات الفلكية
السرعة القطرية (Rv)+9.0[5] كم/ث
الحركة الحقيقية (μ) RA: -441.29[1] mas/yr
Dec.: -215.32[1] mas/س
اختلاف المنظر (π)68.92 ± 0.16[1] mas
المسافةس ض
( ف ن)
القدر المطلق (MV)+2.31[6]
المدار[7]
الرئيسيι UMa A
الرفيقι UMa BC
الدورة (P)2084 ± 15 س
Semimajor axis (a)16.7 ± 0.3"
اختلاف المركز (e)0.90 ± 0.02
ميل (i)54 ± 4°
خط طول العقدة (Ω)134 ± 2°
نقطة التقارب الحقبة (T)B 2029 ± 1
Argument of periastron (ω)
(secondary)		23 ± 5°
التـفـاصـيل
ι UMa Aa
الكتلة1.7 ± 0.1[4] M☉
نصف القطر1.67[8] R☉
الضياء8.98[8] L☉
جاذبية السطح (ج)4.30 ± 0.07[4] س.ج.ث.
درجة الحرارة8,242[9] ك
المعدنية [Fe/H]0.01±0.05[8] العشرية
تسارع الدوران (v sin i)154[10] كم/ث
العمر620[11] م.س.
Bb
الكتلة1±0.3[4][12] M☉
ι UMa B
الكتلة0.35 ± 0.05[4] M☉
نصف القطر0.46[13] R☉
ι UMa C
الكتلة0.30 ± 0.05[4] M☉
نصف القطر0.43[13] R☉
تسميات أخرى
Talitha, ι Ursae Majoris, ι UMa, Iota UMa, 9 Ursae Majoris, BD+48 1707, FK5 335, GJ 331, HD 76644, HIP 44127, HR 3569, SAO 42630, WDS J08592+4803A,BC.[3]
مراجع قواعد البيانات
SIMBADdata
ARICNSdata

القفزة الثالثة الشمالية أو إيوتا الدب الأكبر Iota Ursae Majoris اسمه التقليدي Talitha Borealis مشتق من الاسم العربي، وهو نظام نجمي في كوكبة الدب الأكبر يبعد 47.7 سنة ضوئية عن الأرض.[14] is a star system in the northern circumpolar constellation of Ursa Major. It has an apparent visual magnitude of 3.14,[2] making it visible to the naked eye and placing it among the brighter members of this constellation. Based upon parallax measurements, it is located at a distance of 47.3 light-years (14.5 parsecs) from the Sun.

يتألف هذا النظام النجمي من زوجين من نجم مزدوج النجم الأسطع يعرف بالقفزة الثالث الشمالي A وهو عملاق جزئي أبيض ينتمي إلى الفئة الطيفية A ويملك قدر ظاهري 3.12 أما رفيقه في الثنائية فإنه يدور حوله خلال 4028 يوم.

بينما تدور الثنائية الثانية حول بعضهما البعض خلال 39.7 يوم ويبعدان عن بعضهما حوالي 0.7 ثانية قوسية. بينما يدور الزوجين حول بعضهما البعض كل 818 سنة.

التسمية

ι Ursae Majoris (Latinised to Iota Ursae Majoris) is the star's Bayer designation.

Iota Ursae Majoris in conjunction with comet NEOWISE on 18 July 2020 17° above the north horizon of Berlin

The traditional name Talitha, (which was shared with Kappa Ursae Majoris) comes from the Arabic phrase Al Fiḳrah al Thalitha (عربية: الفقرة الثالثة), a mis-transcription of Al Ḳafzah al Thalitha (عربية: القفزة الثالثة), which means "the third spring, or leap, of the ghazal".[15] The term Borealis meaning "the north side" in Latin. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[16] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[17] included a table of the first two batches of names approved by the WGSN; which included Talitha for this star.

In Chinese, 三台 (Sān Tái), meaning Three Steps, refers to an asterism consisting of ι Ursae Majoris, Kappa Ursae Majoris, Lambda Ursae Majoris, Mu Ursae Majoris, Nu Ursae Majoris and Xi Ursae Majoris. Consequently, the Chinese name for ι Ursae Majoris itself is 上台一 (Shàng Tái yī, إنگليزية: Star of First Upper Step).[18]

The star was also dubbed Dnoces ('Second,' backwards) after Edward H. White II, an Apollo 1 astronaut. The name was invented by his fellow astronaut Gus Grissom as a practical joke.[19]


النظام النجمي

The Iota Ursae Majoris system is composed of two sets of binary stars. The two binary systems orbit around each other once every 2,084 years.[4] The apparent separation between the two binaries is rapidly decreasing as they follow their orbits. In 1841 when the B component was first discovered, they had a separation of 10.7 arcseconds, or at least 156 AU. By 1971 their separation had decreased to 4.5 arcseconds, or at least 66 AU. This system appears to be dynamically unstable with a high likelihood and may become disrupted on a time scale on the order of 105 years.[20]

The brightest component is a white A-type subgiant. It is a member of a spectroscopic binary system whose components have an orbital period of 4,028 days. The companion, which has not been directly observed, is thought to be a white dwarf with a mass of 1.0 ± 0.3 M☉.[4]

The companion binary is composed of the 9th magnitude and 10th magnitude stars, both of which are red dwarfs.[4] These two red dwarfs, designated Iota Ursae Majoris B and C respectively, orbit around each other with a period of 39.7 years, and are separated by roughly 0.7 arcseconds, or at least 10 AU. This pair may be the source of the X-ray emission detected from this system.[21]

انظر أيضا

المراجع

  1. ^ أ ب ت ث ج 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. S2CID 18759600.
  2. ^ أ ب ت ث Johnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99): 99. Bibcode:1966CoLPL...4...99J.
  3. ^ أ ب "iot UMa". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-02-25.
  4. ^ أ ب ت ث ج ح خ د ذ Zhuchkov, R. Ya.; Malogolovets, E. V.; Kiyaeva, O. V.; Orlov, V. V.; Bikmaev, I. F.; Balega, Yu. Yu. (2012). "Physical parameters and dynamical properties of the multiple system ι UMa (ADS 7114)". Astronomy Reports. 56 (7): 512. Bibcode:2012ARep...56..512Z. doi:10.1134/S1063772912070074. S2CID 121681910.
  5. ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities" in IAU Symposium no. 30. 30, University of Toronto: International Astronomical Union. 
  6. ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  7. ^ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 1 August 2017. Retrieved 16 May 2017.
  8. ^ أ ب ت Gáspár, András; Rieke, George H.; Ballering, Nicholas (2016-08-01), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal 826 (2): 171, doi:10.3847/0004-637X/826/2/171, ISSN 0004-637X, Bibcode: 2016ApJ...826..171G  Iota Ursae Majoris' database entry at VizieR.
  9. ^ Draper, Zachary H; Matthews, Brenda; Venn, Kim; Lambert, David; Kennedy, Grant; Sitnova, Tatyana (2018-04-18), "A-type Stellar Abundances: A Corollary to Herschel Observations of Debris Disks", The Astrophysical Journal 857 (2): 93, doi:10.3847/1538-4357/aab1fd, ISSN 0004-637X, Bibcode: 2018ApJ...857...93D 
  10. ^ Royer, F.; Zorec, J.; Gómez, A. E. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics 463 (2): 671–682, doi:10.1051/0004-6361:20065224, Bibcode: 2007A&A...463..671R 
  11. ^ Su, K. Y. L.; Rieke, G. H.; Stansberry, J. A.; Bryden, G.; Stapelfeldt, K. R.; Trilling, D. E.; Muzerolle, J.; Beichman, C. A.; et al. (December 2006), "Debris Disk Evolution around A Stars", The Astrophysical Journal 653 (1): 675–689, doi:10.1086/508649, Bibcode: 2006ApJ...653..675S 
  12. ^ Kirkpatrick, J. Davy; Marocco, Federico; Gelino, Christopher R.; Raghu, Yadukrishna; Faherty, Jacqueline K.; Bardalez Gagliuffi, Daniella C.; Schurr, Steven D.; Apps, Kevin; Schneider, Adam C.; Meisner, Aaron M.; Kuchner, Marc J.; Caselden, Dan; Smart, R. L.; Casewell, S. L.; Raddi, Roberto (2024-04-01). "The Initial Mass Function Based on the Full-sky 20 pc Census of ∼3600 Stars and Brown Dwarfs". The Astrophysical Journal Supplement Series. 271 (2): 55. arXiv:2312.03639. Bibcode:2024ApJS..271...55K. doi:10.3847/1538-4365/ad24e2. ISSN 0067-0049.
  13. ^ أ ب Johnson, H. M.; Wright, C. D. (1983-11-01), "Predicted infrared brightness of stars within 25 parsecs of the sun.", The Astrophysical Journal Supplement Series 53: 643–711, doi:10.1086/190905, ISSN 0067-0049, Bibcode: 1983ApJS...53..643J, https://ui.adsabs.harvard.edu/abs/1983ApJS...53..643J 
  14. ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
  15. ^ Richard Hinckley Allen :Star Names — Their Lore and Meaning - Ursa Major, the Greater Bear
  16. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  17. ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  18. ^ (in صينية) (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 21 日 Archived 2016-03-03 at the Wayback Machine
  19. ^ "Post-landing Activities", Apollo 15 Lunar Surface Journal, NASA, https://history.nasa.gov/alsj/a15/a15.postland.html . Commentary at 105:11:33.
  20. ^ Zhuchkov, R. Ya.; Orlov, V. V.; Rubinov, A. V. (January 2006), "Dynamical stability of the quadruple systems HD 68255/6/7 and HD 76644", Astronomy Reports 50 (1): 62–67, doi:10.1134/S1063772906010070, Bibcode: 2006ARep...50...62Z 
  21. ^ De Rosa, R. J.; Bulger, J.; Patience, J.; Leland, B.; Macintosh, B.; Schneider, A.; Song, I.; Marois, C.; et al. (July 2011), "The Volume-limited A-Star (VAST) survey - I. Companions and the unexpected X-ray detection of B6-A7 stars", Monthly Notices of the Royal Astronomical Society 415 (1): 854–866, doi:10.1111/j.1365-2966.2011.18765.x, Bibcode: 2011MNRAS.415..854D 

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