Astronomy:SU Aurigae
250px Diagram of SU Aurigae's magnetic field | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Auriga |
| Right ascension | 04h 55m 59.38669s[1] |
| Declination | +30° 34′ 01.4996″[1] |
| Apparent magnitude (V) | 9.30[2] |
| Characteristics | |
| Spectral type | G2IIIne[2] |
| Apparent magnitude (G) | 9.25[1] |
| B−V color index | +0.74[3] |
| Variable type | T Tauri |
| Astrometry | |
| Radial velocity (Rv) | 8.31±2.71[1] km/s |
| Proper motion (μ) | RA: 4.185±0.031[1] mas/yr Dec.: −24.304±0.022[1] mas/yr |
| Parallax (π) | 6.3700 ± 0.0303[1] mas |
| Distance | 512 ± 2 ly (157.0 ± 0.7 pc) |
| Absolute magnitude (MV) | +2.83[3] |
| Details[4] | |
| Mass | 2.22+0.02 −0.05 M☉ |
| Radius | 2.61+0.20 −0.23[3] R☉ |
| Luminosity | 12.9±0.3 L☉ |
| Surface gravity (log g) | 3.65±0.01 cgs |
| Temperature | 5680+40 −20 K |
| Metallicity [Fe/H] | +0.48±0.06 dex |
| Rotation | 2.68+0.15 −0.14 days |
| Rotational velocity (v sin i) | 58±3 km/s |
| Age | 2.92+0.19 −0.41 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
SU Aurigae is a T Tauri-type variable star in the constellation Auriga. It is located about 500 light-years (150 parsecs) away in the Taurus-Auriga Star Forming Region. Its apparent magnitude is 9.30, which is dim enough that it cannot be seen with the unaided eye.
In 1907, Henrietta Swan Leavitt discovered that SU Aurigae is a variable star.[5]
SU Aurigae's spectral type of G2IIIne means that it is a G-type star with an effective temperature similar to the Sun. The III in the spectral type refers to its luminosity, which is much higher than normal G-type main sequence stars and would put it in the giant star class.[6] However, it is only about 4 million years old, which is relatively young for a star - young protostars like SU Aurigae are luminous because they are larger, not condensing into a normal size until they are older.[7]
SU Aurigae is known to have a circumstellar protoplanetary disk surrounding it, which is typical of many T Tauri stars.[7] SU Aurigae's disk has a high inclination of 62° and is nearly perpendicular to the plane of sky, so orbiting protoplanets or comets may be the cause of why there are drops in the amount of light detected.[3] SU Aurigae's proper motion and distance is similar to AB Aurigae,[10] a better known pre-main-sequence star, meaning that the two may form a very wide binary system;[6] if not, they are still in the same star association.
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 "SU Aur". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=SU+Aur.
- ↑ 3.0 3.1 3.2 3.3 DeWarf, L. E.; Sepinsky, J. F.; Guinan, E. F.; Ribas, I.; Nadalin, I. (2003). "Intrinsic Properties of the Young Stellar Object SU Aurigae". The Astrophysical Journal 590 (1): 357–367. doi:10.1086/374979. Bibcode: 2003ApJ...590..357D.
- ↑ Mendigutía, I.; Campbell-White, J.; Montesinos, B.; Maldonado, J.; Fullana-García, L.; Mirouh, G. M.; Meeus, G.; Vioque, M. et al. (2026-04-06). "Lithium and the evolution of intermediate-mass T Tauri and Herbig stars. Rotation, accretion, and planets". Astronomy & Astrophysics. doi:10.1051/0004-6361/202659302. ISSN 0004-6361.
- ↑ Leavitt, Henrietta S.; Pickering, Edward C. (July 1907). "71 New Variable Stars in Harvard Maps Nos. 9, 12, 21, 48, and 51". Harvard College Observatory Circular 130 (1–4): 1. Bibcode: 1907HarCi.130....1L. https://articles.adsabs.harvard.edu/pdf/1907HarCi.130....1L. Retrieved 30 November 2024.
- ↑ 6.0 6.1 "AB Aurigae - Jim Kaler". 4 January 2013. http://stars.astro.illinois.edu/sow/abaur.html. Retrieved 17 January 2017.
- ↑ 7.0 7.1 "Encyclopedia of Science: T Tauri star". http://www.daviddarling.info/encyclopedia/T/TTauri.html. Retrieved 17 January 2017.
- ↑ Grankin, K. N.; Shenavrin, V. I.; Irsmambetova, T. R.; Petrov, P. P. (September 2018). "SU Aur: A deep fading event in Visible and near-infrared bands". Information Bulletin on Variable Stars 6253 (1): 1. doi:10.22444/IBVS.6253. Bibcode: 2018IBVS.6253....1G.
- ↑ Cody, Ann Marie; Tayar, Jamie; Hillenbrand, Lynne A.; Matthews, Jaymie M.; Kallinger, Thomas (March 2013). "Precise High-cadence Time Series Observations of Five Variable Young Stars in Auriga with MOST". The Astronomical Journal 145 (3): 79. doi:10.1088/0004-6256/145/3/79. Bibcode: 2013AJ....145...79C. https://ui.adsabs.harvard.edu/abs/2013AJ....145...79C. Retrieved 1 November 2021.
- ↑ van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL.
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