Astronomy:GM Aurigae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Auriga |
| Right ascension | 4h 55m 10.983s |
| Declination | 30° 21' 59.376 |
| Characteristics | |
| Evolutionary stage | T Tauri Star |
| Spectral type | K6V |
| Astrometry | |
| Parallax (π) | 6.264 mas |
| Distance | 505 ly (155 pc) |
| Details | |
| Mass | 0.95 M☉ |
| Radius | 2 R☉ |
| Luminosity | 1.2 L☉ |
| Temperature | 4287 K |
| Age | 3-10 Myr |
| Other designations | |
GM Aur, 2E 0451.9+3017, 2E 1172, 2MASS J04551098+3021595, AAVSO 0448+30, AKARI-IRC-V1 J0455110+302159, AP J04551098+3021595, CSI+30-04520 2, Gaia DR2 156907907082740480, Gaia DR3 156907907082740480, GCRV 55585, GEN# +6.20078077, HBC 77, HBHA 2713-04, IRAS 04519+3017, IRAS C04519+3028, [KW97] 19-51, MHA 259-1, PSCz P04519+3017, SV* SVS 1089, [SW98] 1, TIC 96533063, UCAC4 602-015297, V* GM Aur, WISEA J045510.97+302159.1, WISE J045510.97+302159.2 | |
| Database references | |
| SIMBAD | GM Aur data |
GM Aurigae (GM Aur) is a K6V-type T Tauri star located 155 parsecs from Earth in the constellation of Auriga. It has a mass of 0.95 solar masses, a radius of 2 solar radii, a luminosity of 1.2 solar luminosity and a temperature of 4287 Kelvin. It has an age of around 3-10 million years[1] and is a member of the Taurus-Auriga star forming region. The star is host to a circumstellar disk with a possible planet still forming within it.
It has a stellar rotation period between 5.18 and 6.1 days, with a rotational period of approximately 6.04 days being most likely.
Circumstellar disk
GM Aur is host to an extensively studied circumstellar disk. Within this disk it has a large dust cavity located at 35 AU. There is a fainter disk extending up to 250 AU.[2] There is no consensus on whether this cavity was carved out by a forming exoplanet accreting material, photoevaporation, magnetohydrodynamic disk winds or a combination of all of the above.[3] If there were a planet forming in the system, it would likely have a minimum mass of about 1.10 Jupiter masses.[4] Spatially resolved submillimetre observations of GM Aur confirm the existence of a transitional disc that is inclined at 52.77° with respect to the line of sight. This disk also has an inner dust cavity with a radius of 30-40 AU.[3]
Spectra taken of the stars circumstellar disk show that H2 dominated the spectrum. Other than H2, OH lines have been detected within the disk of GM Aur along with CO emissions. Methyl cations (CH3) and bicarbonate (HCO) have also been found within the disk along with tentative signals of carbon dioxide. Water (H2O) has also been detected, but is photo-destroyed at a rate of around molecules of water destroyed every second. This rate of destruction is less volatile than other stars.[5]
Magnetic field
The large-scale magnetic field of GM Aur has a dipolar configuration with a slight tilt. It has a strength of 730 gauss which is similar to other classical T Tauri stars with similar rotational periods.[3]
References
- ↑ "★ GM Aurigae" (in en). https://www.stellarcatalog.com/stars/gm-aurigae.
- ↑ Macías, Enrique; Espaillat, Catherine C.; Ribas, Álvaro; Schwarz, Kamber R.; Anglada, Guillem; Osorio, Mayra; Carrasco-González, Carlos; Gómez, José F. et al. (2018). "Multiple Rings in the Transitional Disk of GM Aurigae Revealed by VLA and ALMA" (in en). The Astrophysical Journal 865 (1): 37. doi:10.3847/1538-4357/aad811. ISSN 0004-637X. Bibcode: 2018ApJ...865...37M.
- ↑ 3.0 3.1 3.2 B, Zaire; -F, Donati, J; P, Alencar, S; J, Bouvier; C, Moutou; S, Bellotti; A, Carmona; P, Petit et al. (2024-08-29). "Magnetic field, magnetospheric accretion, and candidate planet of the young star GM Aurigae observed with SPIRou" (in en). Monthly Notices of the Royal Astronomical Society 533 (3). doi:10.1093/mnra. ISSN 0035-8711. https://academic.oup.com/mnras/article/533/3/2893/7733099.
- ↑ Zaire, B.; Donati, J.-F.; Alencar, S. P.; Bouvier, J.; Moutou, C.; Bellotti, S.; Carmona, A.; Petit, P. et al. (2024-08-11), "Magnetic field, magnetospheric accretion and candidate planet of the young star GM Aurigae observed with SPIRou", Monthly Notices of the Royal Astronomical Society 533 (3): 2893, doi:10.1093/mnras/stae1955, Bibcode: 2024MNRAS.533.2893Z, http://arxiv.org/abs/2408.05864, retrieved 2025-09-30
- ↑ Romero-Mirza, Carlos E.; Öberg, Karin I.; Banzatti, Andrea; Tabone, Benoît; Najita, Joan; Blake, Geoffrey A.; Bergin, Edwin A.; Krijt, Sebastiaan et al. (2025-09-22). "JWST-MIRI Observations of the Irradiated Chemistry in the Inner Disk Cavity of GM Aur". The Astrophysical Journal 991 (2): 128. doi:10.3847/1538-4357/adf8db. ISSN 0004-637X. Bibcode: 2025ApJ...991..128R.
 |  |
