لاكاي 9352

(تم التحويل من Lacaille 9352)

الإحداثيات: خريطة السماء 23س 05ق 52.03604ث, −35° 51′ 11.0475″

لاكاي 9352
Nearby Stars (14ly Radius).svg
The neighborhood of the Solar System which also includes Lacaille 9352
بيانات الرصـد
الحقبة J2000      اعتدال J2000
الكوكبة Piscis Austrinus
الصعود المستقيم 23س 05د 52.03579ث[1]
الميل −35° 51′ 11.0552″[1]
القدر الظاهري (V)7.34[2]
الخـصـائص
النوع الطيفيM0.5V[3]
U-B دليل الألوان+1.18[2]
B-V دليل الألوان+1.50[2]
النوع المتغيرSuspected[4]
علم القياسات الفلكية
السرعة القطرية (Rv)+8.31±0.13[1] كم/ث
الحركة الحقيقية (μ) RA: +6,765.995 mas/yr
Dec.: +1,330.285 mas/س
اختلاف المنظر (π)304.1354 ± 0.0200[1] mas
المسافةس ض
( ف ن)
القدر المطلق (MV)9.8[5]
التـفـاصـيل
الكتلة0.479+0.011
−0.010[6] M☉
نصف القطر0.474±0.008[6] R☉
الضياء0.0368±0.0006[6] L☉
الحد الداخلي للنطاق الصالح للحياة0.16[7] AU
الحد الخارجي للنطاق الصالح للحياة0.40[7] AU
جاذبية السطح (ج)4.78[8] س.ج.ث.
درجة الحرارة3,672+36
−34[6] ك
المعدنية [Fe/H]−0.22±0.09[9] العشرية
تسارع الدوران (v sin i)1[10] كم/ث
العمر4.57[11] م.س.
تسميات أخرى
HD 217987, CD-36°15693, GCTP 5584, GJ 887, LHS 70, SAO 214301, LTT 9348, LFT 1758, Cordoba 31353, NSV 14420, HIP 114046, UGPMF 591[12]
مراجع قواعد البيانات
SIMBADdata
ARICNSdata
Lacaille 9352 is located in the constellation Piscis Austrinus.
Lacaille 9352 is located in the constellation Piscis Austrinus.
Lacaille 9352
Location of Lacaille 9352 in the constellation Piscis Austrinus

Lacaille 9352 (Lac 9352) is a red dwarf star in the southern constellation of Piscis Austrinus. With an apparent visual magnitude of 7.34,[2] this star is too faint to be viewed with the naked eye except possibly under excellent seeing conditions. Parallax measurements place it at a distance of about 10.74 سنة ضوئية (3.29 فرسخ فلكي) from Earth.[13] It is the eleventh closest star system to the Solar System[14] and is the closest star in the constellation Piscis Austrinus. Its closest neighbour is the EZ Aquarii triple star system at about 4.1 ly away.

Properties

This star has the fourth highest known proper motion,[15] (which was first noticed by Benjamin Gould in 1881[16]) moving a total of 6.9 arcseconds per year. However, this is still a very small movement overall, as there are 3,600 arcseconds in a degree of arc. The space velocity components of this star are (U, V, W) = (−93.9, −14.1, −51.4) km/s.[17] If the radial velocity (Vr) equals +9.7 km/s then about 2,700 years ago Lacaille 9352 was at its minimal distance of approximately 10.63 ly (3.26 pc) from the Sun.[18]

The spectrum of Lacaille 9352 places it at a stellar classification of M0.5V,[3] indicating it is a type of main sequence star known as a red dwarf. This was the first red dwarf star to have its angular diameter measured,[19] with the physical diameter being about 47% of the Sun's radius.[6] It has around half the mass of the Sun[3] and the outer envelope has an effective temperature of about 3,670 K.[6]

Planetary system

In June 2020, two super-Earth planets were reported, as well as a third signal with a period of 50.7 days that may be due to stellar activity—however, if this planet is real it may be located within the habitable zone. They were detected using the radial velocity method from observations with HARPS in Chile and HIRES in Hawaii.[20][21]

Additionally, the star presents a difference on proper motion measurements taken by the Hipparcos and Gaia spacecrafts, suggesting the presence of an outer giant planet.[7]


نظام لاكاي 9352
المرافق
(بالترتيب من النجم) 		الكتلة نصف المحور الرئيسي
(و.ف.) 		الدور المداري
(يوم) 		الانحراف الميل نصف القطر
b ≥ 4.2±0.6 M⊕ 0.068±0.002 9.262±0.001 0.09+0.09
−0.06 		—
c ≥ 7.6±1.2 M⊕ 0.120±0.004 21.789+0.004
−0.005 		0.22+0.09
−0.10 		—
d (unconfirmed) ≳ 8.3 M⊕ ~0.21 ~50.7 0.25+0.20
−0.15 		— —

See also

References

  1. ^ أ ب ت ث قالب:Cite Gaia DR3
  2. ^ أ ب ت ث Cousins, A. W. J. (1973). "UBV photometry of some southern stars". Monthly Notes of the Astronomical Society of Southern Africa. 32: 11. Bibcode:1973MNSSA..32...11C.
  3. ^ أ ب ت Demory, Brice-Olivier; Ségransan, Damien; Forveille, Thierry; Queloz, Didier; Beuzit, Jean-Luc; Delfosse, Xavier; Di Folco, Emmanuel; Kervella, Pierre; Le Bouquin, Jean-Baptiste; Perrier, Christian; Benisty, Myriam; Duvert, Gilles; Hofmann, Karl-Heinz; Lopez, Bruno; Petrov, Romain (October 2009). "Mass-radius relation of low and very low-mass stars revisited with the VLTI". Astronomy and Astrophysics. 505 (1): 205–215. arXiv:0906.0602. Bibcode:2009A&A...505..205D. doi:10.1051/0004-6361/200911976. S2CID 14786643.
  4. ^ Micela, G.; Pye, J.; Sciortino, S. (April 1997). "Coronal properties of nearby old disk and halo dM stars". Astronomy and Astrophysics. 320: 865–877. Bibcode:1997A&A...320..865M.
  5. ^ Murdin, Paul, ed. (November 2000). "Lacaille 9352". Encyclopedia of Astronomy and Astrophysics. Bristol: Institute of Physics Publishing. Bibcode:2000eaa..bookE5158.. doi:10.1888/0333750888/5158. ISBN 0333750888. absolute magnitude is 9.8
  6. ^ أ ب ت ث ج ح Pineda, J. Sebastian; et al. (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal. 918 (1): 23. arXiv:2106.07656. Bibcode:2021ApJ...918...40P. doi:10.3847/1538-4357/ac0aea. S2CID 235435757. 40.
  7. ^ أ ب ت Painter, Katie E.; Bowler, Brendan P.; Franson, Kyle; Becker, Juliette C.; Burt, Jennifer A. (2025-06-26). "Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory". The Astronomical Journal. 170 (3): 147. arXiv:2506.21768. Bibcode:2025AJ....170..147P. doi:10.3847/1538-3881/ade442.
  8. ^ Rabus, Markus; Lachaume, Régis; Jordán, Andrés; Brahm, Rafael; Boyajian, Tabetha; Von Braun, Kaspar; Espinoza, Néstor; Berger, Jean-Philippe; Le Bouquin, Jean-Baptiste; Absil, Olivier (2019). "A discontinuity in the Teff–radius relation of M-dwarfs". Monthly Notices of the Royal Astronomical Society. 484 (2): 2674–2683. arXiv:1901.08077. Bibcode:2019MNRAS.484.2674R. doi:10.1093/mnras/sty3430. S2CID 119189542.
  9. ^ López-Morales, Mercedes (May 2007). "On the Correlation between the Magnetic Activity Levels, Metallicities, and Radii of Low-Mass Stars". The Astrophysical Journal. 660 (1): 732–739. arXiv:astro-ph/0701702. Bibcode:2007ApJ...660..732L. doi:10.1086/513142. S2CID 119530297.
  10. ^ Torres, G. R.; et al. (December 2006). "Search for associations containing young stars (SACY). I. Sample and searching method". Astronomy and Astrophysics. 460 (3): 695–708. arXiv:astro-ph/0609258. Bibcode:2006A&A...460..695T. doi:10.1051/0004-6361:20065602. S2CID 16080025.
  11. ^ Yee, Samuel W.; Petigura, Erik A.; von Braun, Kaspar (2017). "Precision Stellar Characterization of FGKM Stars using an Empirical Spectral Library". The Astrophysical Journal. 836 (1): 77. arXiv:1701.00922. Bibcode:2017ApJ...836...77Y. doi:10.3847/1538-4357/836/1/77. S2CID 6302522.
  12. ^ "LACAILLE 9352 -- Pre-main sequence Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-01-20.
  13. ^ 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.
  14. ^ Research Consortium on Nearby Stars. "The One Hundred Nearest Star Systems". Georgia State University. Archived from the original on 2012-05-13. Retrieved 2010-01-20.
  15. ^ "High Proper Motion Stars in the Hipparcos Catalogue". European Space Agency. July 1, 2007. Retrieved 2010-01-20.
  16. ^ Gould, B. A. (1881). "Corrigenda in the Uranometria Argentina. Star with large proper motion". Astronomische Nachrichten. 100 (1): 7–10. Bibcode:1881AN....100....7G. doi:10.1002/asna.18811000104.
  17. ^ "ARICNS star page of Lacaille 9352". Astronomisches Rechen-Institut Heidelberg. Archived from the original on 2012-09-16. Retrieved 2010-04-16.
  18. ^ "Annotations on NAME LACAILLE 9352 object". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-04-16.
  19. ^ Glindemann, Andreas; Paresce, Francesco. "Giant Eyes for the VLT Interferometer". European Southern Observatory. Retrieved 2010-01-20.
  20. ^ Jeffers, S. V.; Dreizler, S.; Barnes, J. R.; Haswell, C. A.; Nelson, R. P.; Rodríguez, E.; López-González, M. J.; Morales, N.; et al. (2020), "A multiple planet system of super-Earths orbiting the brightest red dwarf star GJ887", Science 368 (6498): 1477–1481, doi:10.1126/science.aaz0795, PMID 32587019, Bibcode: 2020Sci...368.1477J 
  21. ^ Witze, Alexandra (2020). "Why boring could be good for this star's two intriguing planets". Nature. doi:10.1038/d41586-020-01905-5. PMID 34168349. S2CID 220507688. Retrieved 2020-06-30.

قالب:Stars of Piscis Austrinus

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