HD 151804

HD 151804

A light curve for V973 Scorpii, plotted from TESS data[1]
Observation data Epoch J2000.0      Equinox J2000.0
Constellation	Scorpius
Right ascension	16h 51m 33.72181s[2]
Declination	−41° 13′ 49.9195″[2]
Apparent magnitude (V)	5.22 - 5.28[3]
Characteristics
Spectral type	O8 Iaf[4]
U−B color index	−0.838±0.039[5]
B−V color index	0.066±0.013[5]
Variable type	α Cygni[3]
Astrometry
Radial velocity (Rv)	−63±4[6] km/s
Proper motion (μ)	RA: −0.693±0.125[2] mas/yr Dec.: −0.754±0.105[2] mas/yr
Parallax (π)	0.4893 ± 0.1180 mas[2]
Distance	approx. 7,000 ly (approx. 2,000 pc)
Absolute magnitude (MV)	−7.3[7]
Details
Mass	40±5[8] M☉
Radius	35.4±1.2[8] R☉
Luminosity	800000+500000 −300000[8] L☉
Surface gravity (log g)	3.0±0.2[8] cgs
Temperature	29000±500[8] K
Rotational velocity (v sin i)	104±14[9] km/s
Age	2.1[10] Myr
Other designations
V973 Sco, HR 6245, HIP 82493, SAO 227313[11]
Database references
SIMBAD	data

HD 151804, also known as HR 6245 and V973 Scorpii, is a blue supergiant star about 7000 light years from the Earth, in the constellation Scorpius.^[2] It is a 5th magnitude star, so it will be faintly visible to the naked eye of an observer far from city lights. It is a variable star, whose brightness varies slightly from magnitude 5.22 to 5.28, on time scales of a few days.^[3][12] It is one of the brightest stars in the Scorpius OB1 association,^[7] and is located half a degree from NGC 6231,^[13] which is part of the same association.

HD 151804 was determined to be a Wolf-Rayet star sometime between 1888 and 1894 at the Harvard College Observatory.^[14] More modern publications classify it as an Of star, however.^[15]

Photometric observations published by Bart Bok et al. in 1966^[16] and Nancy Morrison in 1975^[17] indicated than HD 151804 might be a variable star. Variability was confirmed by Arnout van Genderen et al. in 1989. They could not deduce a period, but noted that it varied on a timescale of less than two days.^[18] In 1990, HD 151804 was given the variable star designation V973 Scorpii.^[19]

Tahina Ramiaramanantsoa et al. studied HD 151804 in 2015, using the BRITE constellation of nanosatellites. During their two-month period of high cadence observations, they found that the star's brightness varied by 0.04 magnitudes, showing a superposition of a large number of periods, the most pronounced of which were less than one day. These different pulsation modes had lifetimes of five to ten days. They argue that these pulsations may be gravity waves, stochastically excited by the star's convective core.^[20]

In 1968, John Hutchings discovered that HD 151804 has a stellar wind.^[13] It is losing mass at a rate of 6×10⁻⁶M_☉ per year. The wind's terminal velocity is 1450 km/sec.^[8][21]