A light curve for V1040 Scorpii, adapted from Grunhut et al. (2012). [1] The data is from MOST but has been shifted to match the Hipparcos magnitude scale. | |
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Scorpius |
Right ascension | 15h 53m 55.86379s [2] |
Declination | −23° 58′ 41.1434″ [2] |
Apparent magnitude (V) | 5.39 - 5.43 [3] |
Characteristics | |
Spectral type | B2.5V [4] |
Variable type | SX Ari [3] |
Astrometry | |
Proper motion (μ) | RA: −13.406±0.083 [2] mas/yr Dec.: −24.111±0.064 [2] mas/yr |
Parallax (π) | 6.9899 ± 0.0739 mas [2] |
Distance | 467 ± 5 ly (143 ± 2 pc) |
Absolute magnitude (MV) | −0.17 [5] |
Details | |
Mass | 5.5±0.5 [4] M☉ |
Radius | 3.1±0.2 (equatorial) [4] R☉ |
Luminosity | 600+230 −170 [1] L☉ |
Surface gravity (log g) | 4.200±0.053 [6] cgs |
Temperature | 17000±1000 [4] K |
Rotation | 0.508276+0.000015 −0.000012 d [4] |
Rotational velocity (v sin i) | 340±18 [6] km/s |
Age | 206 [7] Myr |
Other designations | |
Database references | |
SIMBAD | data |
HR 5907, also known as V1040 Scorpii and HD 142184, is a star about 470 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. [2] Its brightness varies slightly, ranging from magnitude 5.39 to 5.43 every 12 hours and 20 minutes. [3] HR 5907 is a member of the Scorpius–Centaurus association. [9]
Spectroscopic observations by William Buscombe and Pamela Morris during the years 1956 through 1959 showed that the radial velocity of HR 5907 varied by about 50 km/sec. [10] In 1966, Graham Hill first detected brightness variations in HD 5907. He determined that the brightness varied by 0.03 magnitudes, but was unable to classify the star's type of variability. [11] In 1998, Anne Marie Hubert and Michele Floquet examined the Hipparcos data for the star, confirmed that its brightness varies, and derived a period of 0.508 days with no indications of long-term variability. [12] In 1996 HR 5907 was given the variable star designation V1040 Scorpii. [13]
As of 2018, HR 5907 was the most luminous early spectral type star known at centimeter and millimeter radio wavelengths. [4] On the other end of the electromagnetic spectrum, in 2012 it was clearly detected by the Chandra X-ray Observatory. [14]
HR 5907 is a main sequence star with a strong magnetic field. As of 2018, it had the shortest rotation period known of any early spectral type magnetic star. It spins so rapidly that the star's polar radius is only 88% as large as the equatorial radius. [4] The star has a dipole magnetic field strength of at least 10 kilogauss. [1]
Lambda Scorpii is a triple star system and the second-brightest object in the constellation of Scorpius. It is formally named Shaula; Lambda Scorpii is its Bayer designation, which is Latinised from λ Scorpii and abbreviated Lambda Sco or λ Sco. With an apparent visual magnitude of 1.62, it is one of the brightest stars in the night sky.
13 Andromedae, abbreviated 13 And, is a single, blue-white hued variable star in the northern constellation of Andromeda. 13 Andromedae is the Flamsteed designation, while it bears the variable star designation V388 Andromedae. With a typical apparent visual magnitude of around 5.75, it is dimly visible to the naked eye under good seeing conditions. The distance to this star can be directly estimated from its annual parallax shift of 10.9 mas, yielding a range of 300 light years. At that distance, its brightness is diminished by an extinction of 0.13 magnitude due to interstellar dust. The star is moving closer to the Earth with a heliocentric radial velocity of −8 km/s.
HD 113703, also known by the Bayer designation f Centauri, is a multiple star system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71, which is sufficient to make it faintly visible to the naked eye. The distance to this system is approximately 400 light years based on parallax measurements. It is a member of the Lower Centaurus Crux subgroup of the Scorpius–Centaurus association.
DL Crucis is a variable star in the constellation Crux.
Kappa1 Apodis, Latinized from κ1 Apodis, is the Bayer designation for a binary star system in the southern circumpolar constellation of Apus. Based upon parallax measurements, it is located roughly 1,060 light-years from Earth. The combined apparent visual magnitude of the system is 5.52, indicating that this is a faint, naked eye star that can be viewed in dark suburban skies. It is moving away from the Sun with a radial velocity of +62 km/s.
Chi Ophiuchi, Latinized from χ Ophiuchi, is a variable star in the equatorial constellation of Ophiuchus. It has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.22. The distance to this object, as determined from parallax measurements, is approximately 500 light years, but it is moving closer to the Sun with a radial velocity of −19 km/s. This star is a proper motion member of the Upper Scorpius sub-group in the Scorpius–Centaurus OB association; the nearest such co-moving association of massive stars to the Sun.
HD 93607 is a star in the constellation Carina. Its apparent magnitude is 4.87. Its parent cluster is IC 2602.
f Eridani is a binary, or possibly a triple, star system in the equatorial constellation of Eridanus, consisting of stars HD 24071 and HD 24072. They share a single Hipparcos catalogue entry, HIP 17797, but have separate Bright Star Catalogue listings, HR 1189 and 1190. f Eridani is the Bayer designation of the pair.
KT Lupi is a visual binary star system in the constellation Lupus. It is visible to the naked eye with a combined apparent visual magnitude of 4.55. As of 1983, the pair had an angular separation of 2.19″±0.03″. Based upon an annual parallax shift of 7.6 mas as seen from Earth's orbit, it is located 430 light-years from the Sun. The system is moving further from the Earth with a heliocentric radial velocity of +6.5 km/s. It is a member of the Lower Centaurus–Crux sub-group of the Scorpius–Centaurus association.
QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.
MX Puppis is a class B1.5IV star in the constellation Puppis. Its apparent magnitude varies irregularly between magnitude 4.6 and 4.9 and it is classified as a Gamma Cassiopeiae variable. It is approximately 930 light years away based on parallax.
N Scorpii, also known as HD 148703, is a solitary, bluish-white hued star located in the southern constellation Scorpius. It has an apparent magnitude of 4.23, making it readily visible to the naked eye. N Scorpii was initially given the Bayer designation Alpha Normae by Lacaille but it was later moved from Norma to Scorpius. N Scorpii is currently located 550 light years away based on parallax measurements from the Hipparcos satellite and is part of the Upper Scorpius–Centaurus region of the Scorpius–Centaurus association.
V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8
Y Centauri or Y Cen is a semiregular variable star in the constellation of Centaurus.
V766 Centauri, also known as HR 5171, is a yellow hypergiant in the constellation Centaurus, either 5,000 or 12,000 light years from Earth. It is said to be either an extreme red supergiant (RSG) or recent post-red supergiant (Post-RSG) yellow hypergiant (YHG), both of which suggest it is one of the largest known stars. The star's diameter is uncertain but likely to be between 1,100 and 1,600 times that of the Sun. It was previously thought to be a contact binary, sharing a common envelope of material with a smaller yellow supergiant and secondary star, the two orbiting each other every 1,304 ± 6 days. However this has since been deemed unlikely. An optical companion, HR 5171B, may or may not be at the same distance as the yellow supergiant.
V915 Scorpii is an orange hypergiant variable star in the constellation Scorpius.
QV Andromedae is an Alpha2 Canum Venaticorum variable in the constellation Andromeda. Its maximum apparent visual magnitude is 6.6, so it can be seen by the naked eye under very favourable conditions. The brightness varies slightly following a periodic cycle of approximately 5.23 days.
V2052 Ophiuchi, also known as HR 6684, is a star about 920 light years from Earth in the constellation Ophiuchus. It is a 5th-magnitude star, making it faintly visible to the naked eye of an observer far from city lights. V2052 Ophiuchi is a Beta Cephei variable star, varying slightly in brightness from magnitude 5.81 to 5.84 over a period of about 3.4 hours.
HR 2501, also known as HD 49131 and HP Canis Majoris, is a star about 2,000 light years from the Earth, in the constellation Canis Major. 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 from magnitude 5.35 to 5.80 on a variety of timescales ranging from hours to hundreds of days.
HD 142990, also known as HR 5942 and V913 Scorpii, is a star about 470 light years from the Earth, in the constellation Scorpius. 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 5.40 to 5.47 during its 23.5 hour rotation period. It is a member of the Upper Scorpius Region of the Scorpius–Centaurus association.