Ross 248

Last updated
Ross 248
Andromeda constellation map.svg
Red pog.png
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]

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. [19]

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. [20]

The closest stellar neighbors to Ross 248 are Groombridge 34, at 1.8 light-years away, and Kruger 60, at 4.5 light-years. [21]

See also

Related Research Articles

<span class="mw-page-title-main">Ross 128</span> Small star in constellation of Virgo

Ross 128 is a red dwarf in the equatorial zodiac constellation of Virgo, near β Virginis. The apparent magnitude of Ross 128 is 11.13, which is too faint to be seen with the unaided eye. Based upon parallax measurements, the distance of this star from Earth is 11.007 light-years, making it the twelfth closest stellar system to the Solar System. It was first cataloged in 1926 by American astronomer Frank Elmore Ross.

van Maanen 2 White dwarf

Van Maanen 2, or van Maanen's Star, is the closest known solitary white dwarf to the Solar System. It is a dense, compact stellar remnant no longer generating energy and has equivalent to about 68% of the Sun's mass but only 1% of its radius. At a distance of 14.1 light-years it is the third closest of its type of star after Sirius B and Procyon B, in that order. Discovered in 1917 by Dutch–American astronomer Adriaan van Maanen, Van Maanen 2 was the third white dwarf identified, after 40 Eridani B and Sirius B, and the first solitary example.

HR 7703 is a binary star system in the constellation of Sagittarius. The brighter component has an apparent visual magnitude of 5.31, which means it is visible from suburban skies at night. The two stars are separated by an angle of 7.10″, which corresponds to an estimated semimajor axis of 56.30 AU for their orbit.

TZ Arietis is a red dwarf in the northern constellation of Aries. With a normal apparent visual magnitude of 12.3, it is too faint to be seen by the naked eye, although it lies relatively close to the Sun at a distance of 14.6 light-years. It is a flare star, which means it can suddenly increase in brightness for short periods of time.

<span class="mw-page-title-main">Beta Comae Berenices</span> Star in the constellation Coma Berenices

Beta Comae Berenices is a main sequence dwarf star in the northern constellation of Coma Berenices. It is located at a distance of about 29.95 light-years from Earth. The Greek letter beta (β) usually indicates that the star has the second highest visual magnitude in the constellation. However, with an apparent visual magnitude of 4.3, this star is actually slightly brighter than α Comae Berenices. It can be seen with the naked eye, but may be too dim to be viewed from a built-up urban area.

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

Sigma Boötis, its name Latinized from σ Boötis, is a single star in the northern constellation of Boötes. It has a yellow-white hue and is visible to the naked eye with an apparent visual magnitude of 4.46. Located to the southeast of Rho Boötis, the dwarf Sigma may at first appear as a naked-eye double, but the angular proximity with Rho is merely line-of-sight. Sigma Boötis is located at a distance of 51.1 light years from the Sun based on parallax. The star has a relatively high proper motion and is traversing the sky at the rate of 0.230″ yr−1.

<span class="mw-page-title-main">Theta Cygni</span> Star in the constellation Cygnus

Theta Cygni is a star in the northern constellation of Cygnus. It has an apparent visual magnitude of 4.5, so it can be seen with the naked eye in sufficiently dark skies. Based upon parallax measurements, it is at a distance of about 59.8 light-years from the Earth. It is suspected of hosting an extrasolar planet.

HR 4458 is a binary star system in the equatorial constellation of Hydra. It has the Gould designation 289 G. Hydrae; HR 4458 is the Bright Star Catalogue designation. At a distance of 31.13 light years, it is the closest star system to the Solar System within this constellation. This object is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.97. It is moving closer to the Earth with a heliocentric radial velocity of −22 km/s.

HR 6806 or HD 166620 is a solitary, orange, main sequence, and Sun-like star located thirty-six light-years away, in the constellation Hercules. The star is smaller than the Sun, with around 79% of the solar mass and radius, and 35% of the solar luminosity. It appears to be rotating slowly with an estimated period of 42 days. In 1988, it was noticed that the star had an inactive chromosphere, with a surface magnetic field strength of only 1,500 G. From 1990 activity in the chromosphere increased, inline with a 16 year stellar cycle previously observed. But, sometime after 1994 chromospheric activity greatly reduced, and has stayed flat for more than 16 years. As of 2022, the star appears to have entered the equivalent of a Maunder minimum. The star is around six billion years of age.

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

Gliese 445 is an M-type main sequence star in the northern part of the constellation Camelopardalis.

Xi Pegasi is the Bayer designation for a double star in the northern constellation of Pegasus, the winged horse. Located in the horse's neck, the primary component is an F-type main sequence star that is visible to the naked eye with an apparent visual magnitude of 4.2. It is 86% larger and 17% more massive that the Sun, radiating 4.5 times the solar luminosity. Based upon parallax measurements taken with the Hipparcos spacecraft, it is located 53.2 ± 0.2 light years from the Sun.

Gliese 829 is a double-lined spectroscopic binary system of two red dwarf stars in the constellation of Pegasus. They have a high proper motion of 1.08 arc seconds per year along a position angle of +69.58°. Based upon parallax measurements, the stars are at a distance of about 22 light years from the Sun. The system will make its closest approach to the Sun around 91,000 years from now when it achieves a perihelion distance of 17.65 ly (5.410 pc).

References

  1. 1 2 3 4 5 6 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 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. ↑ 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.
  20. ↑ 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.
  21. ↑ "Ross 248". Sol Station. Retrieved 3 February 2022.

Sources

This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.