Ross 248

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Ross 248
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Ross 248
Location of Ross 248 in the constellation Andromeda

Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 23h 41m 55.03630s [1]
Declination +44° 10′ 38.8189″ [1]
Apparent magnitude  (V)12.23 - 12.34 [2]
Characteristics
Spectral type M6 V [3]
U−B color index +1.48[ citation needed ]
B−V color index +1.92[ citation needed ]
Variable type BY Dra [2]
Astrometry
Radial velocity (Rv)−77.29±0.19 [1]  km/s
Proper motion (μ)RA: 112.527±0.036  mas/yr [1]
Dec.: −1591.650±0.027  mas/yr [1]
Parallax (π)316.4812 ± 0.0444  mas [1]
Distance 10.306 ± 0.001  ly
(3.1597 ± 0.0004  pc)
Absolute magnitude  (MV)14.79 [4]
Details
Mass 0.145 [5]   M☉
Radius 0.190 [5]   R☉
Luminosity 0.0022 [6]   L☉
Surface gravity (log g)5.13 [6]   cgs
Temperature 2,930 [5]   K
Metallicity [Fe/H]+0.23 [5]   dex
Rotation 114.3±2.8  d [7]
Rotational velocity (v sin i)0.1 [8]  km/s
Age 2.6 [5]   Gyr
Other designations
HH Andromedae, HH And, 2MASS J23415498+4410407, G 171-010, GCTP 5736.00, GJ 905, LHS 549. [9]
Database references
SIMBAD data

Ross 248, also called HH Andromedae or Gliese 905, is a small star approximately 10.30 light-years (3.16 parsecs ) [10] from Earth in the northern constellation of Andromeda. Despite its proximity it is too dim to be seen with the naked eye. [11] It was first catalogued by Frank Elmore Ross in 1926 with his second list of proper-motion stars; [12] on which count it ranks 261st in the SIMBAD database. It was too dim to be included in the Hipparcos survey. In about 40,000 years, Voyager 2 will pass 1.7 light-years (9.7 trillion miles) from the star.

Contents

Within the next 80,000 years, Ross 248 is predicted to be the nearest star to the Sun for around 9,000 years, overtaking the current nearest star, the triple system Alpha Centauri.

Characteristics

A visual band light curve for HH Andromedae, adapted from Weis (1994) HHAndLightCurve.png
A visual band light curve for HH Andromedae, adapted from Weis (1994)

This star has about 14% of the Sun's mass and 19% 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 chromospherically-active star. [14] 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 as it rotates, [15] a class known as BY Draconis variables. [2]

Examining the proper motion of Ross 248 has found no evidence of a brown dwarf or stellar companion orbiting between 100–1400 AU, [16] and other unsuccessful searches have been attempted using both the Hubble Space Telescope Wide Field Planetary Camera [4] and by near-infrared speckle interferometry. [17] Long-term observations by the Sproul Observatory show no astrometric perturbations by any unseen companion. [15]

Distance from the Sun

Distances of the nearest stars from 20,000 years ago until 80,000 years in the future Near-stars-past-future-en.svg
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. [10] The trajectory of Ross 248 will bring it closer to the Solar System. In 1993, Matthews projected that in about 33,000 years it would enter a period of about 9,000 years as the closest star to the Sun, as close as 3.024 light-years (0.927 parsecs) in 36,000 years. [18] A more precise estimate in 2022 has it approaching to within 3.048 ly (0.9345 pc) in 36,500 years. [19]

Any future 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 just passes its nearest approach. By comparison, the Voyager 1 has an escape velocity of 16.6 km/s. [20]

Voyager 2 is not headed toward any particular star, although in roughly 42,000 years, it will pass the star Ross 248 at a distance of 1.7 light-years. [21]

The closest stellar neighbors to Ross 248 are the binary systems Groombridge 34, at 1.8 light-years away, and Kruger 60, at 4.5 light-years. [22]

See also

Related Research Articles

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<span class="mw-page-title-main">Groombridge 34</span> Binary star system in the constellation of Andromeda

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<span class="mw-page-title-main">Sigma Boötis</span> Star in the constellation Boötes

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<span class="mw-page-title-main">Theta Persei</span> Star system in the constellation Perseus

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<span class="mw-page-title-main">HD 15115</span> F-type subgiant star in the constellation Cetus

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<span class="mw-page-title-main">Gliese 445</span> Star in the constellation Camelopardalis

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<span class="mw-page-title-main">YZ Canis Minoris</span> Star in the constellation Canis Minor

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<span class="mw-page-title-main">15 Leonis Minoris</span> Star in the constellation Ursa Major

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References

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  2. 1 2 3 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  3. 1 2 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. S2CID   119203469.
  4. 1 2 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 .
  5. 1 2 3 4 5 Mann, Andrew W.; et al. (May 2015). "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius". The Astrophysical Journal. 804 (1): 38. arXiv: 1501.01635 . Bibcode:2015ApJ...804...64M. doi:10.1088/0004-637X/804/1/64. S2CID   19269312. 64.
  6. 1 2 Schweitzer, A.; et al. (2019). "The CARMENES search for exoplanets around M dwarfs. Different roads to radii and masses of the target stars". Astronomy and Astrophysics. 625: 625. arXiv: 1904.03231 . Bibcode:2019A&A...625A..68S. doi:10.1051/0004-6361/201834965.
  7. ↑ Donati, J. -F.; Lehmann, L. T.; Cristofari, P. I.; Fouqué, P.; Moutou, C.; Charpentier, P.; Ould-Elhkim, M.; Carmona, A.; Delfosse, X.; Artigau, E.; Alencar, S. H. P.; Cadieux, C.; Arnold, L.; Petit, P.; Morin, J.; Forveille, T.; Cloutier, R.; Doyon, R.; Hébrard, G.; SLS Collaboration (October 2023). "Magnetic fields and rotation periods of M dwarfs from SPIRou spectra". Monthly Notices of the Royal Astronomical Society. 525 (2): 2015–2039. arXiv: 2307.14190 . Bibcode:2023MNRAS.525.2015D. doi: 10.1093/mnras/stad2301 .
  8. ↑ Newton, Elisabeth R.; Irwin, Jonathan; Charbonneau, David; Berta-Thompson, Zachory K.; Dittmann, Jason A.; West, Andrew A. (2016). "The Rotation and Galactic Kinematics of Mid M Dwarfs in the Solar Neighborhood". The Astrophysical Journal. 821 (2): 93. arXiv: 1511.00957 . Bibcode:2016ApJ...821...93N. doi: 10.3847/0004-637X/821/2/93 . S2CID   89615849.
  9. ↑ "V* HH And". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009-09-06.
  10. 1 2 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.
  11. ↑ Routray, Sudhir K. (2004). Light Years Away: The Whole Creation at a Glance. iUniverse. p. 31. ISBN   0-595-33582-9.
  12. ↑ 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.
  13. 1 2 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. ↑ 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. Vol. 5. Universidad Nacional Autonoma de Mexico. pp. 16–20. Bibcode:1996RMxAC...5...16P.
  15. 1 2 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. S2CID   123491684.
  16. ↑ 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. S2CID   12737223.
  17. ↑ 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.
  18. ↑ 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.
  19. ↑ Bailer-Jones, C. A. L. (August 2022). "Stars That Approach within One Parsec of the Sun: New and More Accurate Encounters Identified in Gaia Data Release 3". The Astrophysical Journal Letters. 935 (1). id. L9. arXiv: 2207.06258 . Bibcode:2022ApJ...935L...9B. doi: 10.3847/2041-8213/ac816a .
  20. ↑ 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.
  21. ↑ Bailer-Jones, Coryn A. L.; Farnocchia, Davide (3 April 2019). "Future stellar flybys of the Voyager and Pioneer spacecraft". Research Notes of the American Astronomical Society. 3 (59): 59. arXiv: 1912.03503 . Bibcode:2019RNAAS...3...59B. doi: 10.3847/2515-5172/ab158e . S2CID   134524048.
  22. ↑ "Ross 248". Sol Station. Retrieved 3 February 2022.

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