Ross 458
Star in the constellation Virgo
From Wikipedia, the free encyclopedia
Ross 458, also referred to as DT Virginis, is a binary star system in the constellation of Virgo. It has an apparent visual magnitude of 9.79[3] and is located at a distance of 37.6 light-years from the Sun. Both of the stars are low-mass red dwarfs with at least one of them being a flare star. This binary system has a circumbinary sub-stellar companion.
Image of Ross 458 with the legacy surveys. The companion is the red object marked with an crosshair in the lower right. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Virgo[1] |
| Right ascension | 13h 00m 46.557s[2] |
| Declination | +12° 22′ 32.68″[2] |
| Apparent magnitude (V) | 9.79[3] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | M0.5 + M7.0[4] |
| U−B color index | 1.12[3] |
| B−V color index | 1.44[3] |
| Astrometry | |
| Radial velocity (Rv) | −12.33±0.32[2] km/s |
| Proper motion (μ) | RA: −628.7±0.184 mas/yr[2] Dec.: −33.5±0.133 mas/yr[2] |
| Parallax (π) | 86.9010±0.1170 mas[2] |
| Distance | 37.53 ± 0.05 ly (11.51 ± 0.02 pc) |
| Absolute magnitude (MV) | +9.47[1] |
| Orbit[5] | |
| Primary | A |
| Name | B |
| Period (P) | 13.63±0.03 yr |
| Semi-major axis (a) | 4.93±0.01 AU |
| Eccentricity (e) | 0.245±0.001 |
| Inclination (i) | 130.3±0.3° |
| Longitude of the node (Ω) | 56.25±0.17° |
| Periastron epoch (T) | 2007.67±0.02 |
| Argument of periastron (ω) (secondary) | 157.5±0.6° |
| Details | |
| A | |
| Mass | 0.553±0.007[5] M☉ |
| Radius | 0.601±0.001[6] R☉ |
| Luminosity | 0.044+0.016 −0.012[7] L☉ |
| Surface gravity (log g) | 4.648+0.001 −0.002[6] cgs |
| Temperature | 3,661.2+2.6 −2.5[6] K |
| Metallicity [Fe/H] | +0.09±0.10[7] dex |
| Rotation | 2.89 d[8] |
| Rotational velocity (v sin i) | 9.6±0.9[9] km/s |
| Age | 400–800[4] Myr |
| B | |
| Mass | 88.9+1.8 −2.8[10] MJup |
| C | |
| Mass | 8.24+0.80 −0.75[6] MJup |
| Radius | 0.85±0.02[6] RJup |
| Luminosity | 5.37+0.08 −0.06×10−6[6] L☉ |
| Surface gravity (log g) | 4.12±0.04[6] cgs |
| Temperature | 771+7 −8[6] K |
| Metallicity | = 0.05+0.03 −0.02[6] |
| Other designations | |
| DT Vir, BD+13°2618, GJ 494, HIP 63510, LHS 2665, LTT 13752, Ross 458, Wolf 462[11] | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| ARICNS | data |
![{\displaystyle {\begin{smallmatrix}\left[{\mathrm {M} }/{\mathrm {H} }\right]\end{smallmatrix}}}](http://wikimedia.org/api/rest_v1/media/math/render/svg/d9a106d03666c72cc54c1dff07a5637d3adda9a1)
Description
This star was mentioned as a suspected variable by M. Petit in 1957.[14] In 1960, O. J. Eggen classified it as a member of the Hyades moving group based on the system's space motion;[15] it is now considered a likely member of the Carina Near Moving Group.[16] Two flares were reported from this star in 1969 by N. I. Shakhovskaya, confirming it as a flare star.[12] It was identified as an astrometric binary in 1994 by W. D. Heintz, who found a period of 14.5 years.[5] The pair were resolved using adaptive optics in 1999.[5] Early mass estimates placed the companion near the substellar limit, and it was initially proposed as a brown dwarf[17] but is now considered late-type red dwarf.[4]
The primary member, component A, is an M-type main-sequence star with a stellar classification of M0.5.[4] It is young, magnetically very active star with a high rate of rotation[17] and strong Hα emission.[4] The star experiences star spots that cover 10–15% of the surface[3] It is smaller and less massive than the Sun. The star is radiating just 4.4%[7] of the luminosity of the Sun from its photosphere at an effective temperature of 3,484 K.[16]
Substellar companion
A distant sub-stellar companion to the binary star system was discovered in 2010 as part of a deep infrared sky survey. This is most likely a T8 spectral type brown dwarf with an estimated rotation period of 6.75±1.58 h. The object varies slightly in brightness, which may be due to patchy clouds.[4] The companion lacks detectable oxygen in the atmosphere, implying its formation from sequestrated source or peculiar atmospheric chemistry.[18] Analysis of its chemical composition show it to be similar to that of Ross 458 A, indicating that the object formed in a stellar-like manner.[6]