An editor has nominated this article for deletion. You are welcome to participate in the deletion discussion , which will decide whether or not to retain it. |
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Carina |
Right ascension | 11h 20m 06.2293s [2] |
Declination | −65° 15′ 07.139″ [2] |
Apparent magnitude (V) | 7.7 - 9.2 [3] |
Characteristics | |
Evolutionary stage | Red supergiant or AGB |
Spectral type | M3 II [4] or M3.8 Ib [5] |
Variable type | SRb [3] |
Astrometry | |
Radial velocity (Rv) | −1.85±0.93 [2] km/s |
Proper motion (μ) | RA: −6.392 [2] mas/yr Dec.: 0.807 [2] mas/yr |
Parallax (π) | 0.215 ± 0.03 mas [6] |
Distance | 14,600+2,200 −1,800 ly (4,486+667 −548 pc) [6] |
Details | |
Radius | 580 [7] [lower-alpha 1] R☉ |
Luminosity | 30,600 [7] L☉ |
Temperature | 3,171 [7] K |
Other designations | |
V538 Carinae, HD 98658, HIP 55355 | |
Database references | |
SIMBAD | data |
V538 Carinae is a variable star in the constellation of Carina, and a possible red supergiant. It is located around 15,000 light-years from Earth. The negative radial velocity of -1.85 km/s show that it is slowly moving towards Earth.
V538 Carinae has a measured angular diameter of 3.4 mas . [8] Its distance is uncertain. At the Hipparcos distance of 1.33±1.08 kpc , this corresponds to a radius of 486 R☉, [7] but at the distance implied by its Gaia Data Release 2 parallax, the radius would be around 1,900 R☉. [8] Calculations based on the Gaia DR2 parallax with temperatures and bolometric corrections inferred from Gaia colours give an even larger radius above 2,200 R☉. [9] However, the DR2 parallax has an excess of astrometric noise larger than the parallax itself, rated at 28.7 [10] where anything above 2 is probably significant, hence affecting the distance and radius measurements. [11]
A Hipparcos distance of 1333 parsecs, together with a luminosity of 30,600 L☉ and a low effective temperature of 3,171 K would correspond to a radius of 580 R☉. [7] [lower-alpha 1] However, the distance has a very high uncertainty of 80%, hence affective the luminosity estimate. [7]
Some studies suggest that this star is a luminous AGB star and a long-period variable, instead of a supergiant. [12] It is classified in the General Catalogue of Variable Stars as a semiregular variable star of type SRb, indicating a cool pulsating giant star, with a possible period of 655 days. Its brightness varies between extremes of magnitude 7.7 and 9.2. [3]
KW Sagittarii is a red supergiant star, located approximately 2,160 parsecs away from the Sun in the direction of the constellation Sagittarius. It is one of the largest known stars, with a diameter about 1,000 times larger than the Sun. If placed at the center of the Solar System, the star's surface would engulf Mars, coming close to Jupiter's orbit.
AG Carinae is a star in the constellation Carina. It is classified as a luminous blue variable (LBV) and is one of the most luminous stars in the Milky Way. The great distance and intervening dust mean that the star is not usually visible to the naked eye; its apparent brightness varies erratically between magnitude 5.7 and 9.0.
HD 161988, also known as HR 6635, is a solitary, orange hued star located in the southern circumpolar constellation Apus. It has an apparent magnitude of 6.07, allowing it to be faintly visible to the naked eye. Parallax measurements place it at a distance of 621 light years, and it is currently receding with a heliocentric radial velocity of 36.8 km/s.
HD 27245, also known as HR 1335 or rarely 25 H. Camelopardalis is a solitary red-hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.4, making it faintly visible to the naked eye. Gaia DR3 Parallax measurements place it approximately 607 light years away from it the Solar System and is drifting further away with a heliocentric radial velocity of 25.2 km/s. At its current distance, HD 27245's brightness is diminished by 0.36 magnitudes due to extinction from interstellar dust. It has an absolute magnitude of −0.27.
Zeta1 Antliae is the Bayer designation for a binary star system in the southern constellation of Antlia. Based upon parallax measurements, the pair are located at a distance of roughly 350 light-years from Earth. They have apparent magnitudes of +6.20 and +7.01 and are separated by 8.042 arcseconds. The apparent magnitude of the combined system is +5.76, which is bright enough to be seen with the naked eye in suitably dark skies.
V602 Carinae is a red supergiant and variable star of spectral type of M3 in the constellation Carina. It is one of largest known stars.
Sigma Ophiuchi, Latinized from σ Ophiuchi, is a single, orange-hued star in the equatorial constellation Ophiuchus. Its apparent visual magnitude is 4.31, which is bright enough to be faintly visible to the naked eye. The annual parallax shift of 3.62 mas as seen from Earth provides a distance estimate of roughly 900 light years. It is moving closer to the Sun with a radial velocity of −28 km/s.
UY Scuti (BD-12°5055) is a red supergiant star, located 5,900 light-years away in the constellation Scutum. It is also a pulsating variable star, with a maximum brightness of magnitude 8.29 and a minimum of magnitude 10.56, which is too dim for naked-eye visibility. It is considered to be one of the largest known stars, with a radius estimated at 909 solar radii, thus a volume of 750 million times that of the Sun. This estimate implies if it were placed at the center of the Solar System, its photosphere would extend past the orbit of Mars or even the asteroid belt.
HD 97413 is a binary star located in the southern constellation Centaurus. The system has a combined magnitude of 6.27, placing it near the limit for naked eye visibility. Based on parallax measurements from the Gaia spacecraft, the system is located 320 light years away from the Solar System.
RX Telescopii is an irregular variable star in the constellation Telescopium. It has a maximum magnitude of 6.45 and a minimum magnitude 7.47. It is a red supergiant with a spectral type of M3Iab, indicating the star is an intermediate-size luminous supergiant star.
RW Cygni is a semiregular variable star in the constellation Cygnus, about a degree east of 2nd magnitude γ Cygni. Its apparent magnitude varies between 8.05 and 9.70 and its spectral type between M3 and M4.
V419 Cephei is an irregular variable star in the constellation of Cepheus with an apparent magnitude that varies between 6.54 and 6.89.
V528 Carinae is a variable star in the constellation Carina.
MZ Puppis is a red supergiant star in the constellation of Puppis. It has a radius of 400 R☉.
QY Puppis is a K-type supergiant star in the constellation of Puppis. With a radius of 515 R☉, it is on the smaller end of the largest known stars.
Y Tauri is a carbon star located in the constellation Taurus. Parallax measurements by Gaia put it at a distance of approximately 2,170 light-years.
36 Camelopardalis is a single star in the northern circumpolar constellation of Camelopardalis. It is visible to the naked eye as a dim point of light with an apparent visual magnitude of +5.3. Parallax measurements provide a distance estimate of approximately 710 light years away from the Sun, and it is drifting away from the Earth with a radial velocity of −1.15 km/s.
HD 193373 is a solitary red hued star located in the equatorial constellation Delphinus. It has an apparent magnitude of 6.21, placing it near the limit for naked eye visibility. Parallax measurements place it 846 light years distant and it is currently receding with a heliocentric radial velocity of 22.7 km/s.
HD 182509, also designated as HR 7370, is an orange hued star located in the southern constellation Telescopium. It has an apparent magnitude of 5.69, making it faintly visible to the naked eye if viewed under ideal conditions. Parallax measurements place the object at a distance of 635 light years. It has a poorly constrained heliocentric radial velocity of −5 km/s, indicating that it is drifting towards the Solar System.
HD 22764, also known as HR 1112, is an orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.78, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of approximately 1,770 light years based on Gaia DR3 parallax measurements but is approaching the Solar System with a heliocentric radial velocity of −12.5 km/s. At its current distance, HD 22764's brightness is diminished by 0.66 magnitudes due to interstellar dust.