IRAS 04125+2902
IRAS 04125+2902 (green star in the middle) and its companion (yellow star below) Credit: Pan-STARRS & Meli thev | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 15m 42.7871s |
| Declination | +29° 09′ 59.832″ |
| Apparent magnitude (V) | 15.487±0.003 |
| Characteristics | |
| Evolutionary stage | Protostar |
| Spectral type | M1.25±0.25 + M6.5 |
| Variable type | T Tauri |
| Astrometry | |
| Radial velocity (Rv) | 13.35±0.39 km/s |
| Proper motion (μ) | RA: +21.811 mas/yr Dec.: −18.145 mas/yr |
| Parallax (π) | 6.2474±0.0270 mas |
| Distance | 522 ± 2 ly (160.1 ± 0.7 pc) |
| Details | |
| Primary | |
| Mass | 0.70±0.04 M☉ |
| Radius | 1.45±0.1 R☉ |
| Luminosity | 0.466±0.041 L☉ |
| Temperature | 4,080±95 K |
| Rotation | 11.31±0.06 d |
| Rotational velocity (v sin i) | 7.1±0.5 km/s |
| Age | 3.3+0.6 −0.5 Myr |
| Companion | |
| Mass | 0.17±0.04 M☉ |
| Radius | 0.96±0.12 R☉ |
| Luminosity | 0.050±0.004 L☉ |
| Temperature | 2,830±90 K |
| Other designations | |
| TIC 56658270, IRAS IRAS 04125+2902, 2MASS J04154278+2909597, WISE J041542.77+290959.5 | |
| Database references | |
| SIMBAD | data |
IRAS 04125+2902 is a M-type star and a T Tauri variable located in the Taurus Molecular Cloud, 160 parsecs (520 light-years) from Earth. This young protostar has 70% of the Sun's mass, 1.45 times the Sun's radius and an effective temperature of 4,080 K (3,810 °C; 6,880 °F). It has a very young age of three million years. It is surrounded by a transitional disk, inclined at 30° relative to Earth, and has one known exoplanet.
It is part of a binary system with 2MASS J04154269+2909558, the two being separated by a projected distance of 635 astronomical units, or 4 arcseconds in the sky. The companion was discovered in 2009, has a spectral type of M6.5, and does not show any infrared excess. Gaia astrometry is similar between 2MASS J04154269+2909558 and IRAS 04125+2902.
The dust disk around IRAS 04125+2902 is truncated, which could be caused by disk evolution or by an eccentric companion. It is unlikely that the wide companion is responsible for the disk truncation, as it's projected distance is much larger than the dust disk's outer limit, but given that the orbital eccentricity of the companion is unknown, this remains plausible.