Ross 614

Coordinates: Sky map 06h 29m 23.401s, −02° 48′ 50.32″
Source: Wikipedia, the free encyclopedia.
Ross 614
Monoceros

Observation data
Epoch J2000      Equinox J2000
Constellation
Monoceros
CCDM J06294-0249 A[1]
Right ascension 06h 29m 23.401s[1]
Declination −02° 48′ 50.32″[1]
Apparent magnitude (V) 11.15[1]
CCDM J06294-0249 B[2]
Right ascension 06h 29m 23.52s[2]
Declination −02° 48′ 51.1″[2]
Apparent magnitude (V) 14.23[2]
Characteristics
Spectral type M4.5V[1]/M8V[2]
Apparent magnitude (B) ~12.77[1]/~15.96[3]
Apparent magnitude (V) ~11.08[1]/~14.23[2]
Apparent magnitude (R) ~9.78[1]
Apparent magnitude (I) ~8.06[1]
Apparent magnitude (J) ~6.376[1]/~8.17[3]
Apparent magnitude (H) ~5.754[1]/~7.38[3]
Apparent magnitude (K) ~5.486[1]/~6.99[3]
U−B color index 1.19/—
B−V color index 1.72/—
Variable type
UV Ceti[4]Flare star[1]
/
Distance
13.36 ± 0.04 ly
(4.10 ± 0.01 pc)
Absolute magnitude (MV)13.09/16.17
Semi-amplitude
(K1)
(primary)		2.201383+0.015629
−0.025186 km/s
Details
Ross 614 A
Mass0.2228 ±0.0055[3] M☉
Ross 614 B
Mass0.1107 ±0.0028[3] M☉
Mass94.837+0.880
−1.370[5] MJup
LHS
1850
Database references
SIMBADThe system
A
B

Ross 614 (V577 Monocerotis) is a

light years
. Because this star is so close to the Earth it is often the subject of study, hence the large number of designations by which it is known.

Binary star system

An ultraviolet band light curve for V577 Monocerotis showing several flares, adapted from Pettersen and Sundland (1991)[6]

This binary star system consists of two closely spaced low-mass red dwarfs. The secondary star is a dim magnitude 14 lost in the glare of the nearby primary star.[2]

A study by

semi-major axis of 4.2 AU, and a very low mass for the companion of 94.8 MJ.[5]

History

The primary star was discovered in 1927 by

E. E. Barnard
, his predecessor at the observatory. Ross then included this new star in his eponymous catalog along with many others he discovered.

The first detection of a binary system was in 1936 by

refractor telescope of the Sproul Observatory.[8] These calculations were used by Walter Baade to find and optically resolve this binary system for the first time using the then new 5 m (200 in) Hale Telescope at the Palomar Observatory in California.[3]

See also

  • List of nearest stars and brown dwarfs

References

  1. ^ a b c d e f g h i j k l m n "V* V577 Mon". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-06-02.
  2. ^ a b c d e f g "LHS 1850". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-06-02.
  3. ^
    S2CID 119597659. Archived from the original
    (PDF) on 2021-12-19. Retrieved 2009-06-03.
  4. ^
    Centre de Données astronomiques de Strasbourg
    . Retrieved 2009-06-02.
  5. ^
    S2CID 251864022
    .
  6. Bibcode:1991A&AS...87..303P
    . Retrieved 29 January 2022.
  7. doi:10.1086/105356
    .
  8. doi:10.1086/106471
    .

Notes

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