Astronomy:GJ 3323

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Short description: Star in the constellation Eridanus

Coordinates: Sky map 05h 01m 57.42611s, −06° 56′ 46.3718″

GJ 3323
GJ 3323 is located in the constellation Eridanus
GJ 3323 is located in the constellation Eridanus

GJ 3323
Location of GJ 3323 in the constellation Eridanus

Observation data
Equinox J2000.0]] (ICRS)
Constellation Eridanus
Right ascension  05h 01m 57.42613s[1]
Declination −06° 56′ 46.3763″[1]
Apparent magnitude (V) 12.20[2]
Characteristics
Spectral type M4.0Ve[3]
B−V color index +1.72[2]
Astrometry
Radial velocity (Rv)42.309±0.0809[2] km/s
Proper motion (μ) RA: −551.746[1] mas/yr
Dec.: −533.648[1] mas/yr
Parallax (π)186.0466 ± 0.0277[1] mas
Distance17.531 ± 0.003 ly
(5.3750 ± 0.0008 pc)
Absolute magnitude (MV)13.57[3]
Details[4]
Mass0.1705±0.0044 M☉
Radius0.1862±0.0059 R☉
Luminosity0.003654±0.000052 L☉
Surface gravity (log g)5.07±0.07 cgs
Temperature3,288±51 K
Metallicity [Fe/H]+0.01±0.16 dex
Rotation88.50 d[5]
Rotational velocity (v sin i)1.0±0.8[3] km/s
Other designations
GJ 3323, LHS 1723, NLTT 14393, 2MASS J05015746-0656459[6]
Database references
SIMBADdata

GJ 3323 (also known as LHS 1723) is a nearby single[7] star located in the equatorial constellation Eridanus, about 0.4° to the northwest of the naked eye star Psi Eridani.[8] It is invisible to the naked eye with an apparent visual magnitude 12.20.[2] Parallax measurements give a distance estimate of 17.5 light-years (5.4 parsecs) from the Sun.[1] It is drifting further away with a radial velocity of +42.3 km/s.[2] Roughly 104,000 years ago, the star is believed to have come to within 7.34 ± 0.16 light-years of the Solar System.[9]

The stellar classification of GJ 3323 is M4.0Ve,[3] indicating that it is a red dwarf, with emission lines appearing in its spectrum.[2] It is fully convective and a source of X-ray emission.[5] The star has 17% of the Sun's mass, 19% of the radius of the Sun, and just 0.4% of the Sun's luminosity.[4]

History of observations

The discovery name of this star is LP 656-38,[10] which indicates that its discovery was published between 1963 and 1981 in University of Minnesota, Minneapolis.[11] "LP" means "Luyten, Palomar".

GJ 3323 is known at least from 1979, when catalogues of high proper motion objects LHS and NLTT were published by Willem Jacob Luyten, and this object was included to these catalogues.[12][13]

Distance measurement

In 1982, Wilhelm Gliese published a photometric distance of GJ 3323 (161 mas),[14] and in 1991 it was included in the 3rd preliminary version of catalogue of nearby stars by Gliese and Jahreiss as NN 3323 (also designated as GJ 3323) with photometric parallax 163.0±26.0 mas.[15]

Its trigonometric parallax remained unknown until 2006, when it was published by the RECONS team. The parallax was 187.92±1.26 mas.[16]

Planetary system

On March 15, 2017, two planets orbiting GJ 3323 were detected by the HARPS telescope, although the discovery team considers GJ 3323 c a planet candidate.[7] The inner planet, GJ 3323b, may orbit within the circumstellar habitable zone of its star.[17][failed verification]

The GJ 3323 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥2.02+0.26
−0.25 M⊕ 		0.03282+0.00054
−0.00056 		5.3636±0.0007 0.23±0.11 — —
c ≥2.31+0.50
−0.49 M⊕ 		0.1264+0.0021
−0.0022 		40.54+0.21
−0.19 		0.17+0.21
−0.12 		— —

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Soubiran, C. et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics 616: A7. doi:10.1051/0004-6361/201832795. Bibcode: 2018A&A...616A...7S. 
  3. ↑ 3.0 3.1 3.2 3.3 Davison, Cassy L. et al. (2015). "A 3D Search for Companions to 12 Nearby M-Dwarfs". The Astronomical Journal 149 (3): 106. doi:10.1088/0004-6256/149/3/106. Bibcode: 2015AJ....149..106D. 
  4. ↑ 4.0 4.1 Schweitzer, A. et al. (May 2019). "The CARMENES search for exoplanets around M dwarfs. Different roads to radii and masses of the target stars". Astronomy & Astrophysics 625: 16. doi:10.1051/0004-6361/201834965. A68. Bibcode: 2019A&A...625A..68S. 
  5. ↑ 5.0 5.1 Wright, Nicholas J. et al. (September 2018). "The stellar rotation-activity relationship in fully convective M dwarfs". Monthly Notices of the Royal Astronomical Society 479 (2): 2351–2360. doi:10.1093/mnras/sty1670. Bibcode: 2018MNRAS.479.2351W. 
  6. ↑ "LP 656-38". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=LP+656-38. 
  7. ↑ 7.0 7.1 Astudillo-Defru, Nicola; Forveille, Thierry; Bonfils, Xavier; Ségransan, Damien; Bouchy, François; Delfosse, Xavier et al. (2017). "The HARPS search for southern extra-solar planets. XLI. A dozen planets around the M dwarfs GJ 3138, GJ 3323, GJ 273, GJ 628, and GJ 3293". Astronomy and Astrophysics 602: A88. doi:10.1051/0004-6361/201630153. Bibcode: 2017A&A...602A..88A. https://www.aanda.org/articles/aa/full_html/2017/06/aa30153-16/aa30153-16.html. 
  8. ↑ Sinnott, Roger W.; Perryman, Michael A. C. (1997). Millennium Star Atlas. 1. Sky Publishing Corporation and the European Space Agency. p. 279. ISBN 0-933346-84-0. 
  9. ↑ Bobylev, V. V. (November 2010). "Stars outside the Hipparcos list closely encountering the Solar system". Astronomy Letters 36 (11): 816–822. doi:10.1134/S1063773710110071. Bibcode: 2010AstL...36..816B. 
  10. ↑ "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal 753 (2): 156. 2012. doi:10.1088/0004-637X/753/2/156. Bibcode: 2012ApJ...753..156K. 
  11. ↑ Dictionary of Nomenclature of Celestial Objects. LP entry. SIMBAD. Centre de Données astronomiques de Strasbourg.
  12. ↑ Luyten, Willem Jacob (1979). "LHS 1723". http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-source=I/87B&LHS=1723. 
  13. ↑ Luyten, Willem Jacob (1979). "NLTT 14393". http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-source=I/98A&recno=14393. 
  14. ↑ Gliese, W. (March 1982). "Photometric parallaxes of nearby main-sequence stars with annual proper motion of 0.7 arcsec or more derived from Eggen's B, V and R, I data". Astronomy and Astrophysics Supplement Series 47: 471–480. Bibcode: 1982A&AS...47..471G. 
  15. ↑ "NN 3323". 1991. http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-source=V/70A&Name=NN%203323. 
  16. ↑ Henry, T. J. et al. (2006). "The Solar Neighborhood. XVII. Parallax Results from the CTIOPI 0.9 m Program: 20 New Members of the RECONS 10 Parsec Sample". The Astronomical Journal 132 (6): 2360–2371. doi:10.1086/508233. Bibcode: 2006AJ....132.2360H. http://repositorio.uchile.cl/bitstream/2250/126230/1/Henry_Todd.pdf. 
  17. ↑ Méndez, Abel; Rivera-Valentín, Edgard G. (2017-02-23). "The Equilibrium Temperature of Planets in Elliptical Orbits". The Astrophysical Journal 837 (1): L1. doi:10.3847/2041-8213/aa5f13. ISSN 2041-8213. Bibcode: 2017ApJ...837L...1M. 



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