IRAS 04125+2902

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[1]
Right ascension 04h 15m 42.7871s[2]
Declination +29° 09′ 59.832″[2]
Apparent magnitude (V) 15.487±0.003[3]
Characteristics
Evolutionary stage pre main sequence[4]
Spectral type M1.25±0.25[3] + M6.5[5]
Variable type T Tauri[6]
Astrometry
Radial velocity (Rv)13.35±0.39[2] km/s
Proper motion (μ) RA: +21.811 mas/yr[2]
Dec.: −18.145 mas/yr[2]
Parallax (π)6.2474±0.0270 mas[2]
Distance522 ± 2 ly
(160.1 ± 0.7 pc)
Details[4]
Primary
Mass0.70±0.04 M☉
Radius1.45±0.1 R☉
Luminosity0.466±0.041 L☉
Temperature4,080±95 K
Rotation11.31±0.06 d
Rotational velocity (v sin i)7.1±0.5 km/s
Age3.3+0.6
−0.5 Myr
Companion
Mass0.17±0.04 M☉
Radius0.96±0.12 R☉
Luminosity0.050±0.004 L☉
Temperature2,830±90 K
Other designations
TIC 56658270, IRAS 04125+2902, 2MASS J04154278+2909597, WISE J041542.77+290959.5
Database references
SIMBADdata

IRAS 04125+2902 is an M-type star and a T Tauri variable[6] located in the Taurus Molecular Cloud, 160 parsecs (520 light-years) from Earth.[4] 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.[4]

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.[4] The companion was discovered in 2009,[7] has a spectral type of M6.5, and does not show any infrared excess.[5]

Circumstellar disk

ALMA image of the dust in the disk.[8]

The disk was first imaged with the Submillimeter Array, which found a disk radius of 50-60 AU and evidence for a narrow dust ring. 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 its 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.[3]

High-resolution images of the disk were taken with ALMA. The dust continuum revealed a ring-gap transitional disk with an inclination of 35.6°. The peak emission of the ring is at a radius of around 37 – 38 AU.[nb 1] Evidence for an inner disk was found, but this could also be free-free emission from the star. If the inner disk exists, the inner and outer disks are misaligned by around 10°. The 12CO gas imaging revealed the rotation of the disk, which was used to estimate the mass of the star at 0.7 – 1.0 M☉. The study found this system to be dynamically complex. Binary orbit, outer disk, inner disk, and planetary orbit are mutually misaligned.[8]

The misalignment might be explained by the dissolution of an unstable triple system. A research team simulated such an ejection interaction for IRAS 01425+2902. An ejected 0.35 M☉ star inclines both the disk and the binary orbit, resulting in a relative misalignment of ≳60° and an highly eccentric orbit (e≳0.5) for the companion star. The planet orbit also becomes inclined relative to the disk.[9]

Planetary system

IRAS 04125+2902 hosts one confirmed exoplanet, IRAS 04125+2902 b, which has an orbital period of nine days around its star, orbiting it closely. It was discovered in 2024 using the transit method and is the youngest transiting exoplanet so far discovered. It is notable as a precursor of super-Earths or sub-Neptunes, commonly found planets. The planet is currently similar to Jupiter in size and its mass is constrained to be less than 0.3 MJ. Over time, it will become a sub-Saturn or sub-Neptune with 60% of its current size or less.[4]

The outer disk is misaligned with the planet and the outer companion, which could be caused by infalling material from the Taurus molecular cloud, but this remains unclear. This misaligment also made it possible to detect IRAS 04125+2902 b via the transit method.[4]

The IRAS 04125+2902 planetary system[3][4]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b <0.3 MJ 0.0813+0.0048
−0.0081 		8.834976(24) — 88.76+0.87
−1.0° 		0.97±0.057 RJ
Wall/Inner edge <18 AU 20° —
Dust disk 20–60 AU <30° —

See also

  • V830 Tauri – Similar to IRAS 04125+2902 and has an unconfirmed planet

Notes

  1. ^ Measured from figure 2 left side.[8]

References

  1. ^ "Finding the constellation which contains given sky coordinates". djm.cc. 2 August 2008. Archived from the original on 15 August 2019. Retrieved 23 May 2024.
  2. ^ a b c d e 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.
  3. ^ a b c d Espaillat, C.; Andrews, S.; Powell, D.; Feldman, D.; Qi, C.; Wilner, D.; D’Alessio, P. (2015-07-09). "The Transitional Disk Around Iras 04125+2902". The Astrophysical Journal. 807 (2): 156. arXiv:1506.01007. Bibcode:2015ApJ...807..156E. doi:10.1088/0004-637x/807/2/156. ISSN 1538-4357.
  4. ^ a b c d e f g h Barber, Madyson G.; Mann, Andrew W.; Vanderburg, Andrew; Krolikowski, Daniel; Kraus, Adam; Ansdell, Megan; Pearce, Logan; Mace, Gregory N.; Andrews, Sean M.; Boyle, Andrew W.; Collins, Karen A.; De Furio, Matthew; Dragomir, Diana; Espaillat, Catherine; Feinstein, Adina D. (November 2024). "A giant planet transiting a 3-Myr protostar with a misaligned disk". Nature. 635 (8039): 574–577. arXiv:2411.18683. Bibcode:2024Natur.635..574B. doi:10.1038/s41586-024-08123-3. ISSN 1476-4687. PMID 39567788.
  5. ^ a b Luhman, K. L.; Mamajek, E. E.; Shukla, S. J.; Loutrel, N. P. (2017-01-01). "A Survey for New Members of the Taurus Star-forming Region with the Sloan Digital Sky Survey". The Astronomical Journal. 153 (1): 46. arXiv:1610.09412. Bibcode:2017AJ....153...46L. doi:10.3847/1538-3881/153/1/46. ISSN 0004-6256.
  6. ^ a b "IRAS 04125+2902". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2024-12-20.
  7. ^ Luhman, K. L.; Mamajek, E. E.; Allen, P. R.; Cruz, K. L. (2009-09-01). "An Infrared/X-Ray Survey for New Members of the Taurus Star-Forming Region". The Astrophysical Journal. 703 (1): 399–419. arXiv:0911.5451. Bibcode:2009ApJ...703..399L. doi:10.1088/0004-637X/703/1/399. ISSN 0004-637X.
  8. ^ a b c Shoshi, Ayumu (2 Sep 2025). "ALMA High-resolution Observation for the Transitional Disk around IRAS 04125+2902". arXiv:2509.01896 [astro-ph.EP].
  9. ^ Nealon, Rebecca; Smallwood, Jeremy L.; Aly, Hossam; Winter, Andrew J.; Longarini, Cristiano; Cuello, Nicolás; Veras, Dimitri; Alexander, Richard (June 2025). "Disc–planet misalignment from an unstable triple system: IRAS04125". Monthly Notices of the Royal Astronomical Society. 540 (1): L84–L90. arXiv:2504.07182. Bibcode:2025MNRAS.540L..84N. doi:10.1093/mnrasl/slaf032. ISSN 0035-8711.
allikas: https://en.wikipedia.org/wiki/IRAS_04125%2B2902