  Ross 614 Location of Ross 614 in the constellationMonoceros | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Monoceros[1] |
| CCDM J06294-0249 A[2] | |
| Right ascension | 06h 29m 23.401s[2] |
| Declination | −02° 48′ 50.32″[2] |
| Apparent magnitude (V) | 11.15[2] |
| CCDM J06294-0249 B[3] | |
| Right ascension | 06h 29m 23.52s[3] |
| Declination | −02° 48′ 51.1″[3] |
| Apparent magnitude (V) | 14.23[3] |
| Characteristics | |
| A | |
| Spectral type | M4.5V[2] |
| Variable type | Flare star (UV Cet)[2] |
| B | |
| Spectral type | M8V[3] |
| Variable type | Flare star (UV Cet)[2] |
| Astrometry | |
| A | |
| Radial velocity (Rv) | 16.70±0.20[2] km/s |
| Proper motion (μ) | RA: +750.14mas/yr[4] Dec.: −802.947mas/yr[4] |
| Parallax (π) | 242.9659±0.8833 mas[4] |
| Distance | 13.42 ± 0.05 ly (4.12 ± 0.01 pc) |
| Absolute magnitude (MV) | 13.09±0.04[5] |
| B | |
| Proper motion (μ) | RA: +707mas/yr[3] Dec.: −703mas/yr[3] |
| Absolute magnitude (MV) | 16.17±0.06[5] |
| Orbit[6] | |
| Period (P) | 16.586±0.004 yr |
| Semi-major axis (a) | 1.1012±0.0082[5]" (4.187+0.008 −0.009 AU) |
| Eccentricity (e) | 0.382±0.0001 |
| Inclination (i) | 52.918±0.016° |
| Longitude of the node (Ω) | 210.385+0.030 −0.031° |
| Periastronepoch (T) | 2445226.863+3.020 −3.043 |
| Argument of periastron (ω) (secondary) | 220.898±0.023° |
| Semi-amplitude (K1) (primary) | 2.201+0.016 −0.025 km/s |
| Details | |
| Ross 614 A | |
| Mass | 0.2228±0.0055[5] M☉ |
| Radius | 0.238±0.017[7] R☉ |
| Luminosity | 0.007[8] L☉ |
| Temperature | 3,193±100[9] K |
| Rotation | ≤2.72+0.74 −0.57[9] days |
| Rotational velocity (v sin i) | 4.73[9] km/s |
| Ross 614 B | |
| Mass | 94.837+0.880 −1.370[6] MJup |
| Radius | 0.11[8][a] R☉ |
| Radius | 74,000 km |
| Luminosity | 0.001[8] L☉ |
| Temperature | 3,145[8] K |
| Other designations | |
| Ross 614, CCDM J06294-0249,GJ 234,GCTP 1509.00,G 106-049,HIP 30920, LFT 473, LPM 239, LTT 2564, NLTT 16580, V577 Monocerotis | |
| Ross 614 A:LHS 1849 | |
| Ross 614 B:LHS 1850 | |
| Database references | |
| SIMBAD | The system |
| A | |
| B | |
Ross 614 (V577 Monocerotis) is ared dwarfUV Ceti[10]flare star and it is the primary member of a nearbybinary star system in the constellation ofMonoceros. It is among thenearest stars at a measured distance of about 13.4light years,[4] but despite this close distance, is invisible to thenaked eye, being ofapparent magnitude 11.[2] 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.
This binary star system consists of two closely spaced low-massred dwarfs. The secondary star is a dimmagnitude 14 lost in the glare of the nearby primary star.[3]
A study byGeorge Gatewood in 2003 using older sources along with data from theHipparcos satellite yielded an orbital period of about 16.6 years and a semi-major axis separation of about 1.1 arc seconds (2.4–5.3 AU).[5] The most recent determination of the system orbital elements comes from a 2022 study combining data fromradial velocity,astrometry, and imaging, which finds a similar orbital period, asemi-major axis of 4.2 AU, and a very low mass for the companion of94.8 MJ.[6]
The primary star was discovered in 1927 byF. E. Ross using the 40 in (100 cm)refractor telescope at theYerkes Observatory. He noticed the highproper motion of this dim 11th magnitude star in his second-epoch plates that were part of anastronomical survey started byE. 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 byDirk Reuyl using the 26-inrefractor telescope of theMcCormick Observatory at theUniversity of Virginia usingastrometric analysis of photographic plates.[12] In 1951Sarah L. Lippincott made the first reasonably accurate predictions of the position of the secondary star using the 24 in (61 cm)refractor telescope of theSproul Observatory.[13] These calculations were used byWalter Baade to find and optically resolve this binary system for the first time using the then new 5 m (200 in)Hale Telescope at thePalomar Observatory inCalifornia.[5]
