Groombridge 1830

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Groombridge 1830
Ursa Major constellation map.svg
Location dot red.svg
The red dot shows the location of Groombridge 1830 in Ursa Major.
HR 4550 Pos.gif
Detailed position of HR 4550 ( = Groombridge 1830; bottom-left edge) related to Chi UMa and Psi UMa.
Observation data
Epoch J2000       Equinox J2000
Constellation Ursa Major
Right ascension 11h 52m 58.76734s [1]
Declination +37° 43′ 07.2541″ [1]
Apparent magnitude  (V)6.44 [2]
Characteristics
Spectral type G8VIp [3]
U−B color index +0.16 [2]
B−V color index +0.75 [2]
Variable type Suspected [4]
Astrometry
Radial velocity (Rv)−98.05±0.12 [1]  km/s
Proper motion (μ)RA: +4002.7  mas/yr [1]
Dec.: −5817.8  mas/yr [1]
Parallax (π)109.0296 ± 0.0197  mas [1]
Distance 29.914 ± 0.005  ly
(9.172 ± 0.002  pc)
Absolute magnitude  (MV)6.64 [5]
Details [6]
Mass 0.63±0.02  M☉
Radius 0.586±0.004  R☉
Luminosity 0.221±0.005  L☉
Surface gravity (log g)4.702±0.015  cgs
Temperature 5,174±32  K
Metallicity [Fe/H]−1.26±0.07  dex
Age 4.7–5.3 [7]   Gyr
Other designations
BD+38 2285, FK5 1307, GCTP 2745.00, GJ 451, HIP 57939, HR 4550, HD 103095, LHS 44, LTT 13276, SAO 62738, 1830 Groombridge, Argelander's Star
Database references
SIMBAD data

Groombridge 1830 (also known as 1830 Groombridge or Argelander's Star) [8] is a star in the constellation Ursa Major.

Contents

Description

It is a yellow-hued class G8 subdwarf catalogued by British astronomer Stephen Groombridge with the Groombridge Transit Circle between 1806 and the 1830s and published posthumously in his star catalog, Catalogue of Circumpolar Stars (1838). Its high proper motion was noted by Friedrich Wilhelm Argelander in 1842.

It is 29.9 light-years (9.2 parsecs ) from the Sun as measured by the Gaia spacecraft, [1] which, as the distance is nearly 10 parsecs, means its absolute magnitude is almost equal to its apparent magnitude. It is a member of the galactic halo; such stars account for only 0.1 to 0.2 percent of the stars near the Sun. Like most halo stars, it has a low abundance of elements other than hydrogen and helium—what astronomers term a metal-poor star. [9]

Once suspected of being a binary star with a period of 175 days, current consensus is that it is single. Previous suspected observations of a stellar companion were probably "superflares"—analogous to the Sun's solar flares, but hundreds to millions of times more energetic. [9] [10] It had one of the first nine identified superflares.

Proper motion

When discovered, it had the highest proper motion of any star known, replacing 61 Cygni in that department. Later it dropped to second place after the discovery of Kapteyn's Star, and still later to third place after the discovery of Barnard's Star. It is considerably farther away than either of those stars, however, which means its transverse velocity is greater.

See also

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References

  1. 1 2 3 4 5 6 7 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 3 Argue, A. N. (1966). "UBV photometry of 550 F, G and K type stars". Monthly Notices of the Royal Astronomical Society. 133 (4): 475–493. Bibcode:1966MNRAS.133..475A. doi: 10.1093/mnras/133.4.475 .
  3. ↑ Johnson, H. L.; Morgan, W. W. (1953). "Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas". Astrophysical Journal. 117: 313–352. Bibcode:1953ApJ...117..313J. doi:10.1086/145697.
  4. ↑ Kukarkin, B. V.; et al. (1981). "Catalogue of suspected variable stars". Nachrichtenblatt der Vereinigung der Sternfreunde. Moscow, USSR: Academy of Sciences. Bibcode:1981NVS...C......0K.
  5. ↑ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv: 0811.3982 , Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID   118577511.
  6. ↑ Karovicova, I.; White, T. R.; Nordlander, T.; Casagrande, L.; Ireland, M.; Huber, D.; Jofré, P. (2020-08-01). "Fundamental stellar parameters of benchmark stars from CHARA interferometry - I. Metal-poor stars". Astronomy & Astrophysics. 640: A25. arXiv: 2006.05411 . Bibcode:2020A&A...640A..25K. doi:10.1051/0004-6361/202037590. ISSN   0004-6361.
  7. ↑ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. arXiv: 0807.1686 . Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID   27151456.
  8. ↑ Peters, C. A. F.; "On the Parallax of Argelander's Star", Monthly Notices of the Royal Astronomical Society, December 1853, v.50, p.302, Bibcode : 1853MNRAS..14...49P
  9. 1 2 "Groombridge 1830". SolStation.
  10. ↑ Rubenstein, Eric P. (February 2001). "Superflares and Giant Planets". American Scientist. 89 (1): 38. arXiv: astro-ph/0101573 . Bibcode:2001AmSci..89...38R. doi:10.1511/2001.1.38. S2CID   119439101.
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