HP Tauri
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 35m 52.78s[1] |
| Declination | +22° 54′ 23.2″[1] |
| Apparent magnitude (V) | 14.90[2] |
| Characteristics | |
| Evolutionary stage | Pre-main-sequence star |
| Spectral type | K2-5e[3] |
| Variable type | Orion variable |
| Astrometry | |
| Proper motion (μ) | RA: +9.037[1] mas/yr[1] Dec.: −13.853[1] mas/yr[1] |
| Parallax (π) | 5.8395±0.0490 mas |
| Distance | 559 ± 5 ly (171 ± 1 pc) |
| Details | |
| Mass | 1.21[4] M☉ |
| Radius | 1.60[4] R☉ |
| Luminosity | 0.99[4] L☉ |
| Surface gravity (log g) | 3.98[5] cgs |
| Temperature | 4,522[5] K |
| Rotation | 4.33 days[6] |
| Rotational velocity (v sin i) | 17.3[7] km/s |
| Age | 1[8] Myr |
| Other designations | |
| HP Tau, EPIC 247592463, IRAS 04328+2248, 2MASS J04355277+2254231, Gaia DR3 145213187879627776 | |
| Database references | |
| SIMBAD | data |
HP Tauri is a star system in the constellation of Taurus.[9] The component stars of the system are HP Tau, HP Tau G2, and HP Tau G3.[10] HP Tauri is a T Tauri variable star.[10] The star system is located in the Taurus molecular cloud[9] and nebula GN 04.32.8.[11] HP Tauri is around 550 light-years (170 parsecs) away from the Solar System.[12][13] The system is around five-million-years-old.[13]
Observation history
In 1979, HP Tau was found to be surrounded by several stars, HP Tau G1 (which is not gravitationally bound to the rest of the system), HP Tau G2, and HP Tau G3.[13] HP Tau G3 was found to be a binary system in of itself in 1994.[13]
Properties
HP Tau G2 is a G-type star with a surface temperature of 6,030 K (5,760 °C; 10,390 °F).[13][14] HP Tau G2 has elevated iron levels compared to stars later in their evolutions.[15] The star has non-thermal radio pulses.[13]
HP Tau G3 is a M-type, tight binary star.[13][14] HP Tauri may possess a non-thermal spectrum.[16]
References
- ^ 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.
- ^ Ducati, J. R. (August 2002). "VizieR Online Data Catalog: Stellar Photometry in Johnson's 11-color system (Ducati, 2002)". VizieR Online Data Catalog. 2237: II/237. Bibcode:2002yCat.2237....0D.
- ^ Hartigan, Patrick; Strom, Karen M.; Strom, Stephen E. (June 1994). "Are Wide Pre--Main-Sequence Binaries Coeval?". The Astrophysical Journal. 427: 961. Bibcode:1994ApJ...427..961H. doi:10.1086/174203. ISSN 0004-637X.
- ^ a b c Manzo-Martínez, Ezequiel; Calvet, Nuria; Hernández, Jesús; Lizano, Susana; Hernández, Ramiro Franco; Miller, Christopher J.; Maucó, Karina; Briceño, César; d'Alessio, Paola (2020). "The Evolution of the Inner Regions of Protoplanetary Disks". The Astrophysical Journal. 893 (1): 56. arXiv:2004.02916. Bibcode:2020ApJ...893...56M. doi:10.3847/1538-4357/ab7ead.
- ^ a b Saad, Serat; Lane, Kaitlyn; Kounkel, Marina; Stassun, Keivan G.; López-Valdivia, Ricardo; Kim, Jinyoung Serena; Peña Ramírez, Karla; Stringfellow, Guy S.; Román-Zúñiga, Carlos G.; Hernández, Jesús; Wolk, Scott J.; Hillenbrand, Lynne A. (2024). "ABYSS. II. Identification of Young Stars in Optical SDSS Spectra and Their Properties". The Astronomical Journal. 167 (3): 125. arXiv:2401.01932. Bibcode:2024AJ....167..125S. doi:10.3847/1538-3881/ad2001.
- ^ Long, Liu; Bi, Shaolan; Zhang, Jinghua; Zhang, Xianfei; Zhang, Liyun; Ge, Zhishuai; Li, Tanda; Chen, Xunzhou; Li, Yaguang; Ye, Lifei; Sun, Tiancheng; Zhou, Jianzhao (2023). "Investigating 16 Open Clusters in the Kepler/K2-Gaia DR3 Field. I. Membership, Binary Systems, and Rotation". The Astrophysical Journal Supplement Series. 268 (1): 30. arXiv:2307.06596. Bibcode:2023ApJS..268...30L. doi:10.3847/1538-4365/ace5af.
- ^ Flores, C.; Connelley, M. S.; Reipurth, B.; Duchêne, G. (2022). "The Effects of Starspots on Spectroscopic Mass Estimates of Low-mass Young Stars". The Astrophysical Journal. 925 (1): 21. arXiv:2111.03957. Bibcode:2022ApJ...925...21F. doi:10.3847/1538-4357/ac37bd.
- ^ Ward-Duong, K.; Patience, J.; Bulger, J.; Van Der Plas, G.; Ménard, F.; Pinte, C.; Jackson, A. P.; Bryden, G.; Turner, N. J.; Harvey, P.; Hales, A.; De Rosa, R. J. (2018). "The Taurus Boundary of Stellar/Substellar (TBOSS) Survey. II. Disk Masses from ALMA Continuum Observations". The Astronomical Journal. 155 (2): 54. arXiv:1712.07669. Bibcode:2018AJ....155...54W. doi:10.3847/1538-3881/aaa128.
- ^ a b "The young stars of Taurus". ESA Hubble. 2025-06-30. Retrieved 2026-01-19.
- ^ a b "Hubble Views the Dawn of a Sun-like Star". NASA Science. Retrieved 2026-01-21.
- ^ "The Young Stars of Taurus". SETI Institute. 2025-12-01. Retrieved 2026-01-22.
- ^ "Triple Stellar Treat". NOIRLab. University of Alaska Anchorage. Retrieved 2026-01-25.
- ^ a b c d e f g Torres, Rosa M.; Loinard, Laurent; Mioduszewski, Amy J.; Rodríguez, Luis F. (2009-05-19). "VLBA DETERMINATION OF THE DISTANCE TO NEARBY STAR-FORMING REGIONS. III. HP TAU/G2 AND THE THREE-DIMENSIONAL STRUCTURE OF TAURUS". The Astrophysical Journal. 698 (1): 242–249. arXiv:0903.5338. doi:10.1088/0004-637X/698/1/242. ISSN 0004-637X – via IOP Science.
- ^ a b Rizzuto, Aaron C.; Dupuy, Trent J.; Ireland, Michael J.; Kraus, Adam L. (2020-02-01). "Dynamical Masses of Young Stars. II. Young Taurus Binaries Hubble 4, FF Tau, and HP Tau/G3". The Astrophysical Journal. 889 (2): 175. arXiv:1911.12378. Bibcode:2020ApJ...889..175R. doi:10.3847/1538-4357/ab5aed. ISSN 0004-637X.
- ^ Telleschi, A.; Güdel, M.; Briggs, K. R.; Audard, M.; Scelsi, L. (2007-06-01). "High-resolution X-ray spectroscopy of T Tauri stars in the Taurus-Auriga complex". Astronomy & Astrophysics. 468 (2): 443–462. arXiv:astro-ph/0611024. Bibcode:2007A&A...468..443T. doi:10.1051/0004-6361:20066193. ISSN 0004-6361 – via EDP Sciences.
- ^ Pudritz, R.E. (1986-05-06). "Star formation in molecular disks". Publications of the Astronomical Society of the Pacific. 98 (606): 709. Bibcode:1986PASP...98..709P. doi:10.1086/131818 – via IOP Science.