HD 283572

HD 283572

A combined y band (near-infrared) and visual band light curve for V987 Tauri, adapted from Strassmeier and Rice (1998)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 04h 21m 58.8483s[2]
Declination +28° 18′ 06.5119″[2]
Characteristics
Evolutionary stage pre-main-sequence star[3]
Spectral type G5[4]
Apparent magnitude (B) 9.80[2]
Apparent magnitude (g) 8.80[5]
Apparent magnitude (R) 9.14[2]
Apparent magnitude (J) 7.414[2]
Variable type T Tau[4]
Astrometry
Radial velocity (Rv)15.0±1.5[4] km/s
Proper motion (μ) RA: 8.84±0.03 mas/yr[5]
Dec.: -26.426±0.017 mas/yr[5]
Parallax (π)7.8735 ± 0.0190 mas[5]
Distance414.2 ± 1.0 ly
(127.0 ± 0.3 pc)
Details[4]
Mass1.6 M☉
Radius2.2 R☉
Luminosity5.5 L☉
Temperature5770 K
Metallicity [Fe/H]0.7±0.2[3] dex
Rotation1.55 d[3]
Rotational velocity (v sin i)78[3] km/s
Age9 Myr
Other designations
HDE 283572, 2MASS J04215884+2818066, BD+27 657, GSC 01828-00481, HIP 20388, TYC 1828-481-1, V987 Tauri, Gaia DR2 164536250037820160
Database references
SIMBADdata

HD 283572 is a young T Tauri-type pre-main sequence star in the constellation of Taurus about 414 light years away, belonging to the Taurus Molecular Cloud.[3] It is a rather evolved protostar which already dispersed its birth shroud.[4] The star emits a very high X-ray flux of 1031 ergs/s. That radiation flux associated with the magnetic activity induced a high coronal temperature of 3 kEv and regular flares.[6] HD 283572 will eventually evolve to an A-type main-sequence star when on the main sequence.[3] It is no longer accreting mass, and is magnetically decoupled from the remnants of the protoplanetary disk,[3] belonging to the terminal, 3rd phase of the disk evolution.[7] Submillimeter Array (SMA) 1.3mm observations of HD 283572 detected an extreme brightening event with a radio luminosity of 8.3x1016erg/s/Hz that spanned 9 hours on January 17th 2022.[8][9] Although HD 283572 was observed by the SMA on 8 separate nights, millimeter emission was detected on one night only, strongly suggesting stellar variability as a result of an extreme stellar flare.[8][9]

  1. ^ Cite error: The named reference Strassmeier was invoked but never defined (see the help page).
  2. ^ a b c d e Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  3. ^ a b c d e f g Scelsi, L.; Maggio, A.; Peres, G.; Pallavicini, R. (2005), "Coronal properties of G-type stars in different evolutionary phases", Astronomy & Astrophysics, 432 (2): 671–685, arXiv:astro-ph/0501631, Bibcode:2005A&A...432..671S, doi:10.1051/0004-6361:20041739, S2CID 15298988
  4. ^ a b c d e Torres, Rosa M.; Loinard, Laurent; Mioduszewski, Amy J.; Rodriguez, Luis F. (2007), "VLBA Determination of the Distance to Nearby Star-forming Regions. II. Hubble 4 and HDE 283572 in Taurus", The Astrophysical Journal, 671 (2): 1813–1819, arXiv:0708.4403, Bibcode:2007ApJ...671.1813T, doi:10.1086/522924, S2CID 16357104
  5. ^ a b c Cite error: The named reference EDR3 was invoked but never defined (see the help page).
  6. ^ Favata, F.; Micela, G.; Sciortino, S. (1998), "X-ray spectroscopy of the weak-lined T Tauri star HD 283572", Astronomy and Astrophysics, 336: 413–420, Bibcode:1998A&A...337..413F
  7. ^ Yasui, Chikako; Hamano, Satoshi; Fukue, Kei; Kondo, Sohei; Sameshima, Hiroaki; Takenaka, Keiichi; Matsunaga, Noriyuki; Ikeda, Yuji; Kawakita, Hideyo; Otsubo, Shogo; Watase, Ayaka; Taniguchi, Daisuke; Mizumoto, Misaki; Izumi, Natsuko; Kobayashi, Naoto (2019), "Possible Progression of Mass-flow Processes around Young Intermediate-mass Stars Based on High-resolution Near-infrared Spectroscopy. I. Taurus", The Astrophysical Journal, 886 (2): 115, arXiv:1909.09850, Bibcode:2019ApJ...886..115Y, doi:10.3847/1538-4357/ab45ee, S2CID 202718804
  8. ^ a b Cite error: The named reference Lovell2024 was invoked but never defined (see the help page).
  9. ^ a b Extreme Eruption on Young Sun-like Star Signals Savage Environment for Developing Exoplanets