A light curve for V833 Tauri. The main plot (adapted from Strassmeier et al. [1] and Oláh et al. [2] ) shows the long term visual band variation, and the inset plot (plotted from TESS data [3] ) shows the periodic variability. | |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Taurus |
Right ascension | 04h 36m 48.2413s [4] |
Declination | 27° 07′ 55.8983″ [4] |
Apparent magnitude (V) | 8.02 - 8.40 [5] |
Characteristics | |
Evolutionary stage | Main sequence |
Spectral type | K5Ve [6] |
B−V color index | 1.12 [6] |
Variable type | BY Dra + Flare [5] |
Astrometry | |
Radial velocity (Rv) | 42±3 [7] km/s |
Proper motion (μ) | RA: 232.17±0.06 mas/yr [7] Dec.: -147.48±0.04 mas/yr [7] |
Parallax (π) | 57.49 ± 0.05 mas [7] |
Distance | 56.73 ± 0.05 ly (17.39 ± 0.02 pc) |
Details [6] | |
Mass | 0.8 M☉ |
Radius | 0.8 R☉ |
Surface gravity (log g) | 4.5 cgs |
Temperature | 4250±100 K |
Rotational velocity (v sin i) | 7.4 km/s |
Age | 1 [8] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
HD 283750, also known as V833 Tauri, is a K-type main-sequence star 57 light-years away from the Sun. The star is much younger than the Sun's at 1 billion years. [8] HD 283750 is similar to the Sun in its concentration of heavy elements. [6]
The star has a co-moving white dwarf companion WD 0443+270 at a projected separation of 124″, [9] both possibly ejected members of the Hyades cluster. The white dwarf companion has a rather exotic iron core [8] and belongs to spectral class DA9 and has the mass of 0.62±0.02M☉. [10]
Although HD 283750 was classified as a multi-period variable, [11] a paper in 2020 claims its variability is not exceeding the variability of the Sun, and no period can be identified. [12]
HD 283750 is covered by a large amount of starspots, filling up to 28% of the stellar surface at the maxima of the magnetic cycle. [13] In November 1993, the star emitted an extremely powerful flare with energy of 7.47×1034 ergs, which is on or even above the upper limit of possible energy releases in flare stars. [11] The flares of HD 283750 are accompanied by particle beams strong enough to affect the polarization properties of the stellar photosphere. [14]
In 1996 a suspected 50-MJ brown dwarf HD 283750b on a 1.79-day orbit around HD 283750 was detected by the differential Doppler spectroscopy method. By 2007, the mass of the companion was refined to 0.19M☉, making it a red dwarf star. [15]
Zeta Andromedae is a star system in the constellation Andromeda. It is approximately 189 light-years from Earth.
HD 4308 is a single star in the southern constellation of Tucana. It has a yellow hue and is a challenge to view with the naked eye even under good seeing conditions, having an apparent visual magnitude of 6.54. This object is located at a distance of 72 light years, as determined from parallax measurements. It is a population II star and is considered to be a member of the thick disk. The star is receding from the Sun with a radial velocity of +95 km/s.
HD 4628 is a main sequence star in the equatorial constellation of Pisces. It has a spectral classification of K2.5 V and an effective temperature of 5,055 K, giving it an orange-red hue with a slightly smaller mass and girth than the Sun. HD 4628 lies at a distance of approximately 24.3 light years from the Sun based on parallax. The apparent magnitude of 5.7 is just sufficient for this star to be viewed with the unaided eye. The star appears to be slightly older than the Sun—approximately 5.4 billion years in age. The surface activity is low and, based upon the detection of UV emission, it may have a relatively cool corona with a temperature of one million K.
AB Doradus is a pre-main-sequence quadruple star system in the constellation Dorado. The primary is a flare star that shows periodic increases in activity.
EQ Virginis is a single variable star in the equatorial constellation of Virgo. It has a baseline visual apparent magnitude of 9.36, but is a flare star that undergoes sporadic bursts of brightening. The star is located at a distance of 67 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −23 km/s. It is a member of the IC 2391 moving group of stars, which is between 30 and 50 million years old.
DT Virginis, also known as Ross 458, is a binary star system in the constellation of Virgo. It has an apparent visual magnitude of 9.79 and is located at a distance of 37.6 light-years from the Sun. Both of the stars are low-mass red dwarfs with at least one of them being a flare star. This binary system has a circumbinary sub-stellar companion.
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111 Tauri is a wide binary star system in the constellation Taurus. It is located at a distance of 48 light years from the Sun. Primary component A is a main sequence star with a stellar classification of F8V. The secondary component B is a K-type main sequence star. The primary is larger and more luminous than the Sun, with about 130% of the Sun's radius and 185% of the Sun's luminosity. The apparent magnitude of 5.0 indicates it is a faint star that can be viewed by the naked eye under good, dark-sky conditions.
90 Tauri is a star in the zodiac constellation of Taurus, located 144 light-years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.27. 90 Tauri is a member of the Hyades cluster and is listed as a double star.
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XX Trianguli, abbreviated XX Tri, is a variable star in the northern constellation of Triangulum, about 1.5° to the WNW of Beta Trianguli along the constellation border with Andromeda. It is classified as a RS Canum Venaticorum variable and ranges in brightness from magnitude 8.1 down to 8.7, which is too faint to be visible to the naked eye. The system is located at a distance of approximately 642 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −26 km/s.
9 Ceti is a star in the equatorial constellation of Cetus. It has the variable star designation BE Ceti, while 9 Ceti is the Flamsteed designation. It has an apparent visual magnitude of 6.4, which is below the limit that can be seen with the naked eye by a typical observer. Based upon parallax measurements, this star is 69.6 light years away from the Sun.
HK Aquarii is a single variable star in the equatorial constellation of Aquarius. It is invisible to the naked eye, having an average apparent visual magnitude that fluctuates around 10.99. The star is located at a distance of 81 light years from the Sun based on parallax. The radial velocity is poorly constrained but it appears to be drifting further away at a rate of ~2 km/s.
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HD 111395 is a single, variable star in the northern constellation of Coma Berenices. It has the variable star designation LW Com, short for LW Comae Berenices; HD 111395 is the Henry Draper Catalogue designation. The star has a yellow hue and is just bright enough to be barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.29. Based upon parallax measurements, it is located at a distance of 55.8 light years from the Sun. The star is drifting closer with a radial velocity of −8.9 km/s. It is a member of the Eta Chamaeleontis stellar kinematic group.
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HD 283572 is a young T Tauri-type pre-main sequence star in the constellation of Taurus about 414 light years away, belonging to the Taurus Molecular Cloud. It is a rather evolved protostar which already dispersed its birth shroud. The star emits a very high X-ray flux of 1031 ergs/s. That radiation flux associated with the magnetic activity induced a high coronal temperature of 3 kEv and regular flares. HD 283572 will eventually evolve to an A-type main-sequence star when on the main sequence. It is no longer accreting mass, and is magnetically decoupled from the remnants of the protoplanetary disk, belonging to the terminal, 3rd phase of the disk evolution.
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