HD 201852

HD 201852
Location of HD 201852 on the map (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Microscopium
Right ascension 21h 13m 18.96155s[1]
Declination −36° 25′ 24.7016″[1]
Apparent magnitude (V) 5.95±0.01[2]
Characteristics
Spectral type K0 III[3]
U−B color index +0.74[4]
B−V color index +0.98[4]
Astrometry
Radial velocity (Rv)0.4±0.4[5] km/s
Proper motion (μ) RA: +33.411 mas/yr[1]
Dec.: +3.122 mas/yr[1]
Parallax (π)8.9286 ± 0.038 mas[1]
Distance365 ± 2 ly
(112.0 ± 0.5 pc)
Absolute magnitude (MV)+0.73[6]
Details
Mass1.87[7] M☉
Radius9.89±0.50[8] R☉
Luminosity58.0±0.5[1] L☉
Surface gravity (log g)2.80±0.08[9] cgs
Temperature4,984±34[10] K
Metallicity [Fe/H]−0.02±0.03[11] dex
Rotational velocity (v sin i)<1.0[12] km/s
Age1.58[7] Gyr
Other designations
57 G. Microscopii[13], CD−36°14676, CPD−36°9343, GC 29648, HD 201852, HIP 104752, HR 8108, SAO 212800, TIC 159690250[14]
Database references
SIMBADdata

HD 201852 (HR 8108; 57 G. Microscopii) is a solitary star located in the southern constellation Microscopium. It is faintly visible to the naked eye as an orange-hued point of light with an apparent magnitude of 5.95.[2] Gaia DR3 parallax measurements imply a distance of 365 light-years[1] and it is slowly receding with a heliocentric radial velocity of 0.4 km/s.[5] At its current distance, HD 201852's brightness is diminished by an interstellar extinction of 0.11 magnitudes[15] and it has an absolute magnitude of +0.73.[6]

HD 201852 has a stellar classification of K0 III,[3] indicating that it is an evolved K-type giant that has exhausted hydrogen at its core and left the main sequence. It has 1.87 times the mass of the Sun but at the age of 1.58 billion years,[7] it has expanded to 9.89 times the radius of the Sun.[8] It radiates 58 times the luminosity of the Sun[1] from its enlarged photosphere at an effective temperature of 4,984 K.[10] HD 201852 has a near solar metallicity at [Fe/H] = −0.02[11] and it spins too slowly for its projected rotational velocity to be measured accurately; it has been given an upper limit of 1 km/s.[12] Based on its kinematics and elemental abundances, HD 201852 is said to be part of the thin disk population.[16]

  1. ^ a b c d e f g Cite error: The named reference GaiaDR3 was invoked but never defined (see the help page).
  2. ^ a b Cite error: The named reference Tycho2000 was invoked but never defined (see the help page).
  3. ^ a b Cite error: The named reference Houk1982 was invoked but never defined (see the help page).
  4. ^ a b Cite error: The named reference Oja1970 was invoked but never defined (see the help page).
  5. ^ a b Cite error: The named reference Gontcharov2006 was invoked but never defined (see the help page).
  6. ^ a b Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  7. ^ a b c Cite error: The named reference Bertelli1994 was invoked but never defined (see the help page).
  8. ^ a b Cite error: The named reference Kervella2004 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Ottoni2022 was invoked but never defined (see the help page).
  10. ^ a b Cite error: The named reference Luck2015 was invoked but never defined (see the help page).
  11. ^ a b Cite error: The named reference Alves2015 was invoked but never defined (see the help page).
  12. ^ a b Cite error: The named reference De Medeiros2014 was invoked but never defined (see the help page).
  13. ^ Cite error: The named reference Gould1879 was invoked but never defined (see the help page).
  14. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  15. ^ Cite error: The named reference Gontcharov2017 was invoked but never defined (see the help page).
  16. ^ Cite error: The named reference Adibekyan2015 was invoked but never defined (see the help page).