HD 21071

HD 21071

A light curve for V576 Persei, plotted from Hipparcos data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 03h 25m 57.382s[2]
Declination +49° 07′ 14.73″[2]
Apparent magnitude (V) 6.09[3]
Characteristics
Evolutionary stage Main sequence
Spectral type B7 V[4]
B−V color index −0.073±0.005[3]
Variable type SPB[5]
Astrometry
Radial velocity (Rv)−1.5±0.9[6] km/s
Proper motion (μ) RA: +23.753 mas/yr[2]
Dec.: −26.656 mas/yr[2]
Parallax (π)6.0959 ± 0.0444 mas[2]
Distance535 ± 4 ly
(164 ± 1 pc)
Absolute magnitude (MV)−0.19[3]
Details
Mass3.69+0.14
−0.15[5] M☉
Radius2.21[7] R☉
Luminosity278.0+53.1
−44.7[5] L☉
Surface gravity (log g)4.30[4] cgs
Temperature14,768[4] K
Metallicity [Fe/H]0.0082+0.0053
−0.0032[5] dex
Rotational velocity (v sin i)58[4] km/s
Age90[4] Myr
Other designations
V576 Per, BD+48° 913, GC 4075, HD 21071, HIP 15988, HR 1029, SAO 38817[8]
Database references
SIMBADdata

HD 21071 is a blue-white hued variable star in the northern constellation of Perseus. Also known as V576 Persei, it is a sixth magnitude star that is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 6.09.[3] The brightness of the star varies with a multiperiodic cycle.[9] The distance to HD 21071, as determined from an annual parallax shift of 6.1 mas,[2] is 535 light years. It is a member of the young Alpha Persei cluster, Melotte 20,[4][10] and moving is closer to the Earth with a heliocentric radial velocity of −1.5 km/s.[6]

This is a B-type main-sequence star with a stellar classification of B7 V.[4] HD 21071 belongs to an unusual stellar population termed 'sn' stars. These seem to be related to chemically peculiar stars, but have sharp ('s') Balmer and metal absorption lines with "broad coreless He I" ('n') lines. The latter wide, "nebulous" lines may be due to Stark broadening caused by an electric field.[4] HD 21071 is a slowly pulsating B-type star (SPB star) that was initially found to vary with a period of 0.84 days. Further study revealed four frequencies, with the two dominant, higher amplitude frequencies having similar cycles of 1.19 and 1.15 per day.[5]

Pulsation Periods[5]
ID Frequency
(d−1) 		V Amplitude
(mmag) 		Radial Velocity
(km/s)
1 1.18843 18.5 3.28±0.85
2 1.14934 7.7 –
3 1.41968 3.8 –
4 0.95706 3.0 –

Stellar models show the star to have 3.7[5] times the mass of the Sun, with 2.21[7] times the Sun's radius. It is 90[4] million years old with a near-solar metallicity and is spinning with a projected rotational velocity of 58 km/s.[4] The star is radiating 278[5] times the Sun's luminosity from its photosphere at an effective temperature of 14,768 K.[4]

  1. ^ Cite error: The named reference HIPCurve was invoked but never defined (see the help page).
  2. ^ a b c d e Cite error: The named reference GaiaEDR3 was invoked but never defined (see the help page).
  3. ^ a b c d Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  4. ^ a b c d e f g h i j k Cite error: The named reference Saffe2014 was invoked but never defined (see the help page).
  5. ^ a b c d e f g h Cite error: The named reference Szewczuk2015 was invoked but never defined (see the help page).
  6. ^ a b Cite error: The named reference Gontcharov2006 was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Mathias2001 was invoked but never defined (see the help page).
  8. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Samus2017 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference Zuckerman2012 was invoked but never defined (see the help page).