A white-light light curve light curve for HL Tau 76, adapted from Warner and Nather (1972)[1]
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS)
Constellation
Taurus
Right ascension
04h 18m 56.638s[2]
Declination
+27° 17′ 48.31″[2]
Apparent magnitude (V)
14.1–15.28[3]
Characteristics
Spectral type
DA4.3[4]
B−V color index
0.2[5]
Variable type
DAV (ZZ Ceti)[3]
Astrometry
Proper motion (μ)
RA: 62.600[2] mas/yr Dec.: −72.819[2] mas/yr
Parallax (π)
20.7244 ± 0.0338 mas[2]
Distance
157.4 ± 0.3 ly (48.25 ± 0.08 pc)
Absolute magnitude (MV)
11.69[4]
Details
Mass
0.575±0.005[6]M☉
Radius
0.0162[6]R☉
Luminosity
0.00389[6]L☉
Surface gravity (log g)
7.8[7] cgs
Temperature
11,375±30[6] K
Other designations
EGGR 265, V411 Tau, WD 0416+272[5]
Database references
SIMBAD
data
HL Tau 76 is a variable white dwarf star of the DAV (or ZZ Ceti) type. It was observed by G. Haro and W. J. Luyten in 1961,[8][9] and was the first variable white dwarf discovered when, in 1968, Arlo U. Landolt found that it varied in brightness with a period of approximately 749.5 seconds, or 12.5 minutes.[9] Like other DAV white dwarfs, its variability arises from non-radial gravity wave pulsations within itself.[10], § 7. Later observation and analysis has found HL Tau 76 to pulsate in over 40 independent vibrational modes, with periods between 380 seconds and 1390 seconds.[11]
The designation HL Tau 76 derives from the discovery of this star as a white dwarf, when it was described as Taurus no.76 in a publication authored by Guillermo Haro and Willem Jacob Luyten.[8] The exact designation HL Tau 76 was then used in subsequent papers, including one giving the star its designation EGGR 265 where it was noted to be variable.[12] It was then included in the 57th name-list of variable stars and given the variable star designation V441 Tauri.[13] The unusual designation HL Tau 76 continues to be used by most authors.[14]
^Cite error: The named reference Warner was invoked but never defined (see the help page).
^ abcdeBrown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
^ abCombined General Catalogue of Variable Stars (GCVS), v. 4.2. CDS ID II/250.
^ abGianninas, A.; Bergeron, P.; Ruiz, M. T. (2011). "A Spectroscopic Survey and Analysis of Bright, Hydrogen-rich White Dwarfs". The Astrophysical Journal. 743 (2): 138. arXiv:1109.3171. Bibcode:2011ApJ...743..138G. doi:10.1088/0004-637X/743/2/138. S2CID 119210906.
^ ab"HL Tau 76". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved June 12, 2007.
^ abcdPech, D.; Vauclair, G.; Dolez, N. (2006). "Asteroseismological constraints on the structure of the ZZ Ceti star HL Tau 76". Astronomy and Astrophysics. 446 (1): 223. Bibcode:2006A&A...446..223P. doi:10.1051/0004-6361:20053150.
^Gentile Fusillo, N. P.; Tremblay, P. -E.; Cukanovaite, E.; Vorontseva, A.; Lallement, R.; Hollands, M.; Gänsicke, B. T.; Burdge, K. B.; McCleery, J.; Jordan, S. (2021). "A catalogue of white dwarfs in Gaia EDR3". Monthly Notices of the Royal Astronomical Society. 508 (3): 3877. arXiv:2106.07669. Bibcode:2021MNRAS.508.3877G. doi:10.1093/mnras/stab2672.
^ abHaro, G.; Luyten, W. J. (1961). "Nueva estrella enana blanca en las nubes obscuras del Toro". Boletín de los Observatorios de Tonantzintla y Tacubaya. 3: 35. Bibcode:1961BOTT....3...35H.
^ abLandolt, Arlo U. (1968). "A New Short-Period Blue Variable". The Astrophysical Journal. 153: 151. Bibcode:1968ApJ...153..151L. doi:10.1086/149645.
^Koester, D.; Chanmugam, G. (1990). "Physics of white dwarf stars". Reports on Progress in Physics. 53 (7): 837. Bibcode:1990RPPh...53..837K. doi:10.1088/0034-4885/53/7/001. S2CID 250915046.
^Dolez, N.; et al. (2006). "Whole Earth telescope observations of the ZZ Ceti star HL Tau 76" (PDF). Astronomy and Astrophysics. 446 (1): 237. Bibcode:2006A&A...446..237D. doi:10.1051/0004-6361:20053149.
^Greenstein, Jesse L. (October 1969). "The Lowell Suspect White Dwarfs". Astrophysical Journal. 158: 281. Bibcode:1969ApJ...158..281G. doi:10.1086/150191.
^Kukarkin, B. V.; et al. (October 1970). "57th Name-List of Variable Stars". Information Bulletin on Variable Stars. 480 (1): 1. Bibcode:1970IBVS..480....1K.
^Chen, Y. H.; Shu, H. (January 2021). "Asteroseismology of the DAV star R808". Monthly Notices of the Royal Astronomical Society. 500 (4): 4703–4709. arXiv:2011.06918. Bibcode:2021MNRAS.500.4703C. doi:10.1093/mnras/staa3572.
HLTau76 is a variable white dwarf star of the DAV (or ZZ Ceti) type. It was observed by G. Haro and W. J. Luyten in 1961, and was the first variable...
failed to observe this.: §7.1.1 The first variable white dwarf found was HLTau76; in 1965 and 1966, and was observed to vary with a period of approximately...
1960s failed to observe this. The first variable white dwarf found was HLTau76; in 1965 and 1966, Arlo U. Landolt observed it to vary with a period of...
discovered the first intrinsically variable white dwarf when he found that HLTau76 varied in brightness with a period of approximately 749.5 seconds, or...
Arlo U. Landolt when he observed in 1965 and 1966 that the luminosity of HLTau76 varied with a period of approximately 12.5 minutes. 1968 Up quark The...
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