Astronomy:Lacaille 9352

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Short description: Star in the constellation Piscis Austrinus

Coordinates: Sky map 23h 05m 52.03604s, −35° 51′ 11.0475″

Lacaille 9352
Nearby Stars (14ly Radius).svg
the neighborhood of the solar system which also includes Lacaille 9352
Observation data
Equinox J2000.0]] (ICRS)
Constellation Piscis Austrinus
Right ascension  23h 05m 52.03604s[1]
Declination −35° 51′ 11.0475″[1]
Apparent magnitude (V) 7.34[2]
Characteristics
Spectral type M0.5V[3]
U−B color index +1.18[2]
B−V color index +1.50[2]
Variable type Suspected[4]
Astrometry
Radial velocity (Rv)+9.7[5] km/s
Proper motion (μ) RA: +6,765.995[6] mas/yr
Dec.: +1,330.388[6] mas/yr
Parallax (π)304.1354 ± 0.0200[7] mas
Distance10.7241 ± 0.0007 ly
(3.2880 ± 0.0002 pc)
Absolute magnitude (MV)9.8[8]
Details
Mass0.479+0.011
−0.010[9] M☉
Radius0.474±0.008[9] R☉
Luminosity0.0368±0.0006[9] L☉
Surface gravity (log g)4.78[10] cgs
Temperature3,672+36
−34[9] K
Metallicity [Fe/H]−0.22±0.09[11] dex
Rotational velocity (v sin i)1[5] km/s
Age4.57[12] Gyr
Other designations
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[13]
Database references
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 light-years (3.29 parsecs) from Earth.[1] It is the eleventh closest star system to the Solar System[14] and is the closest star in the constellation Piscis Austrinus. The ChView simulation[15] shows that 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,[16] (which was first noticed by Benjamin Gould in 1881[17]) 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.[18] 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.[19]

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,[20] with the physical diameter being about 47% of the Sun's radius.[9] It has around half the mass of the Sun[3] and the outer envelope has an effective temperature of about 3,670 K.[9]

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.[21][22]

The Lacaille 9352 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
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. ↑ 1.0 1.1 1.2 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 2.3 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. ↑ 3.0 3.1 3.2 Demory, Brice-Olivier; Ségransan, Damien; Forveille, Thierry; Queloz, Didier; Beuzit, Jean-Luc; Delfosse, Xavier; Di Folco, Emmanuel; Kervella, Pierre 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. 
  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. ↑ 5.0 5.1 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. doi:10.1051/0004-6361:20065602. Bibcode: 2006A&A...460..695T. 
  6. ↑ 6.0 6.1 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  7. ↑ Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  8. ↑ Murdin, Paul, ed (November 2000). Encyclopedia of Astronomy and Astrophysics. Bristol: Institute of Physics Publishing. doi:10.1888/0333750888/5158. ISBN 0333750888. Bibcode: 2000eaa..bookE5158.. "absolute magnitude is 9.8". 
  9. ↑ 9.0 9.1 9.2 9.3 9.4 9.5 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. doi:10.3847/1538-4357/ac0aea. 40. Bibcode: 2021ApJ...918...40P. 
  10. ↑ Rabus, Markus; Lachaume, Régis; Jordán, Andrés; Brahm, Rafael; Boyajian, Tabetha; Von Braun, Kaspar; Espinoza, Néstor; Berger, Jean-Philippe et al. (2019). "A discontinuity in the Teff–radius relation of M-dwarfs". Monthly Notices of the Royal Astronomical Society 484 (2): 2674–2683. doi:10.1093/mnras/sty3430. Bibcode: 2019MNRAS.484.2674R. 
  11. ↑ 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. doi:10.1086/513142. Bibcode: 2007ApJ...660..732L. 
  12. ↑ 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. doi:10.3847/1538-4357/836/1/77. Bibcode: 2017ApJ...836...77Y. 
  13. ↑ "LACAILLE 9352 -- Pre-main sequence Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+217987. 
  14. ↑ Research Consortium on Nearby Stars. "The One Hundred Nearest Star Systems". Georgia State University. http://www.chara.gsu.edu/RECONS/TOP100.posted.htm. 
  15. ↑ "Solstation and ChView". http://www.solstation.com/. 
  16. ↑ "High Proper Motion Stars in the Hipparcos Catalogue". European Space Agency. July 1, 2007. http://www.rssd.esa.int/index.php?project=HIPPARCOS&page=hpm. 
  17. ↑ Gould, B. A. (1881). "Corrigenda in the Uranometria Argentina. Star with large proper motion". Astronomische Nachrichten 100 (1): 7–10. doi:10.1002/asna.18811000104. Bibcode: 1881AN....100....7G. https://zenodo.org/record/1424713. 
  18. ↑ "ARICNS star page of Lacaille 9352". Astronomisches Rechen-Institut Heidelberg. http://www.ari.uni-heidelberg.de/datenbanken/aricns/cnspages/4c01887.htm. 
  19. ↑ "Annotations on NAME LACAILLE 9352 object". SIMBAD. Centre de Données astronomiques de Strasbourg. http://cdsannotations.u-strasbg.fr/annotations/simbadObject/1191721. 
  20. ↑ Glindemann, Andreas; Paresce, Francesco. "Giant Eyes for the VLT Interferometer". European Southern Observatory. http://www.eso.org/public/news/eso0134/. 
  21. ↑ 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 
  22. ↑ 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. https://www.nature.com/articles/d41586-020-01905-5. Retrieved 2020-06-30. 

External links



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