Ross 248

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Ross 248
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension  23h 41m 55.0361s[1]
Declination +44° 10′ 38.825″[1]
Apparent magnitude (V) 12.29[2]
Spectral type M6 V[3]
Apparent magnitude (J) 12.3[2]
U−B color index +1.48[2]
B−V color index +1.92[2]
Variable type Flare star
Radial velocity (Rv)–75.2 ± 3.7[4] km/s
Proper motion (μ) RA: 112.692±0.153[1] mas/yr
Dec.: −1592.055±0.112[1] mas/yr
Parallax (π)316.9558 ± 0.1260[1] mas
Distance10.290 ± 0.004 ly
(3.155 ± 0.001 pc)
Absolute magnitude (MV)14.79[5]
Mass0.136[3] M
Radius0.16[6] R
Luminosity0.0018[7] L
Surface gravity (log g)5.12[8] cgs
Temperature2,799[8] K
Rotational velocity (v sin i)1.2[3] km/s
Other designations
HH Andromedae, HH And, 2MASS J23415498+4410407, G 171-010, GCTP 5736.00, GJ 905, LHS 549.[2]
Database references

Ross 248, also called HH Andromedae or Gliese 905, is a small star located approximately 10.30 light-years (3.16 parsecs)[9] from Earth in the northern constellation of Andromeda. Despite its proximity to the Earth, this star is too dim to be seen with the naked eye.[10] Ross 248 was first catalogued by Frank Elmore Ross in 1926 with his second list of proper-motion stars.[11] In the SIMBAD database it is the 261st-highest proper-motion star. It was too dim to be included in the Hipparcos survey.


This star has about 12% of the Sun's mass and 16% of the Sun's radius, but only 0.2% of the Sun's luminosity. It has a stellar classification of M6 V,[3] which indicates it is a type of main-sequence star known as a red dwarf. This is a flare star that occasionally increases in luminosity.[12] With high probability, there appears to be a long-term cycle of variability with a period of 4.2 years. This variability causes the star to range in visual magnitude from 12.23 to 12.34.[13] In 1950, this became the first star to have a small variation in magnitude attributed to spots on its photosphere.[14]

Long-term observations of this star by the Sproul Observatory show no astrometric perturbations by an unseen companion.[14] The proper motion of this star was examined for a brown dwarf or stellar companion orbiting at a wide separation (between 100–1400 AU) but none was found.[15] A search for a faint companion using the Hubble Space Telescope Wide Field Planetary Camera revealed nothing,[5] nor did a search with near-infrared speckle interferometry.[16]

Distance from the Sun[edit]

Distances of the nearest stars from 20,000 years ago until 80,000 years in the future

The space velocity components of this star in the galactic coordinate system are [U, V, W] = [–32.9 ± 0.7, –74.3 ± 1.3, 0.0 ± 1.4] km/s.[9] The trajectory of Ross 248 will bring it closer to the Solar System in the future. In 1993, Matthews suggested that in about 33,000 years Ross 248 would be the closest star to the Sun, approaching within a minimum distance of 3.024 light-years (0.927 parsecs) in 36,000 years.[17] However, it will recede thereafter and will again be further from the Sun than Proxima Centauri 42,000 years from now.[17]

A spacecraft that escaped the Solar System with a velocity of 25.4 km/s would reach this star 37,000 years from now, when the star is just past its nearest approach. By comparison, the Voyager 1 has an escape velocity of 16.6 km/s.[18]

Field star[edit]

The star PLX 5735 is located nearly along the line of sight to Ross 248, but it is not physically associated.

Name PLX 5735
Right ascension  23h 41m 54s
Declination +44° 14′ 00″
Apparent magnitude (V) 12.6
Spectral type A5
Database references Simbad

See also[edit]


  1. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d e "V* HH And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-09-06.
  3. ^ a b c d Jenkins, J. S.; Ramsey, L. W.; Jones, H. R. A.; Pavlenko, Y.; Gallardo, J.; Barnes, J. R.; Pinfield, D. J. (October 2009), "Rotational Velocities for M Dwarfs", The Astrophysical Journal, 704 (2): 975–988, arXiv:0908.4092, Bibcode:2009ApJ...704..975J, doi:10.1088/0004-637X/704/2/975
  4. ^ Deshpande, R.; Martín, E. L.; Montgomery, M. M.; Osorio, M. R. Zapatero; Rodler, F.; Burgo, C. del; Bao, N. Phan; Lyubchik, Y.; Tata, R.; Bouy, H.; Pavlenko, Y. (2012). "Intermediate Resolution Near-infrared Spectroscopy of 36 Late M Dwarfs". The Astronomical Journal. 144 (4): 99. arXiv:1207.2781. Bibcode:2012AJ....144...99D. doi:10.1088/0004-6256/144/4/99. ISSN 1538-3881. Retrieved 10 May 2018.
  5. ^ a b Schroeder, Daniel J.; et al. (2000). "A Search for Faint Companions to Nearby Stars Using the Wide Field Planetary Camera 2". The Astronomical Journal. 119 (2): 906–922. Bibcode:2000AJ....119..906S. doi:10.1086/301227.
  6. ^ Johnson, H. M.; Wright, C. D. (November 1983). "Predicted infrared brightness of stars within 25 parsecs of the Sun". Astrophysical Journal Supplement Series. 53: 643–711, 705. Bibcode:1983ApJS...53..643J. doi:10.1086/190905.
  7. ^ West, Frederick R. (June 1999). "Monitoring Nearby Stars for Transits by Extrasolar Jovial Planets, II: Transits of M-Type (Red) Dwarf Stars by Close Extrasolar Giant (Jovian) Planets". The Journal of the American Association of Variable Star Observers. 27 (1): 77–78. Bibcode:1999JAVSO..27...77W.
  8. ^ a b Cenarro, A. J.; et al. (2007). "Medium-resolution Isaac Newton Telescope Library of Empirical Spectra – II. The Stellar Atmospheric Parameters". Monthly Notices of the Royal Astronomical Society. 374 (2): 664–690. arXiv:astro-ph/0611618. Bibcode:2007MNRAS.374..664C. doi:10.1111/j.1365-2966.2006.11196.x.
  9. ^ a b Leggett, S. K. (September 1992). "Infrared colors of low-mass stars". Astrophysical Journal Supplement Series. 82 (1): 351–394. Bibcode:1992ApJS...82..351L. doi:10.1086/191720.
  10. ^ Routray, Sudhir K. (2004), Light Years Away: The Whole Creation at a Glance, iUniverse, p. 31, ISBN 0-595-33582-9
  11. ^ Ross, Frank E. (February 1926). "New proper-motion stars, (second list)". Astronomical Journal. 36 (856): 124–128. Bibcode:1926AJ.....36..124R. doi:10.1086/104699.
  12. ^ Poveda, Arcadio; Allen, Christine; Herrera, Miguel Angel (1996). "Chromospheric Activity, Stellar Winds and Red Stragglers". Workshop on Colliding Winds in Binary Stars to Honor Jorge Sahade. 5. Universidad Nacional Autonoma de Mexico. pp. 16–20.
  13. ^ Weis, Edward W. (March 1994). "Long term variability in dwarf M stars". Astronomical Journal. 107 (3): 1135–1140. Bibcode:1994AJ....107.1135W. doi:10.1086/116925.
  14. ^ a b Lippincott, S. L. (July 1978). "Astrometric search for unseen stellar and sub-stellar companions to nearby stars and the possibility of their detection". Space Science Reviews. 22 (2): 153–189. Bibcode:1978SSRv...22..153L. doi:10.1007/BF00212072.
  15. ^ Hinz, Joannah L.; et al. (February 2002). "A Near-Infrared, Wide-Field, Proper-Motion Search for Brown Dwarfs". The Astronomical Journal. 123 (4): 2027–2032. arXiv:astro-ph/0201140. Bibcode:2002AJ....123.2027H. doi:10.1086/339555.
  16. ^ Leinert, C.; Henry, T.; Glindemann, A.; McCarthy, D. W. Jr. (September 1997). "A search for companions to nearby southern M dwarfs with near-infrared speckle interferometry". Astronomy and Astrophysics. 325: 159–166. Bibcode:1997A&A...325..159L.
  17. ^ a b Matthews, R. A. J. (Spring 1994). "The Close Approach of Stars in the Solar Neighborhood". Quarterly Journal of the Royal Astronomical Society. 35 (1): 1. Bibcode:1994QJRAS..35....1M.
  18. ^ West, F. R. (March 1985). "A Suggested Future Space Mission to the Low-Luminosity Star Ross 248=Gliese 905". Bulletin of the American Astronomical Society. 17: 552. Bibcode:1985BAAS...17..552W.



External links[edit]