HD 283750

Last updated
HD 283750
V833TauLightCurve.png
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
V833 Tauri, BD+26 730, Gaia DR2  151650076838458112, GJ  171.2, HIP  21482, TYC  1838-564-1, 2MASS J04364822+2707559 [4]
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]

Suspected substellar companion

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]

Related Research Articles

<span class="mw-page-title-main">Hyades (star cluster)</span> Open cluster in the constellation Taurus

The Hyades is the nearest open cluster and one of the best-studied star clusters. Located about 153 light-years away from the Sun, it consists of a roughly spherical group of hundreds of stars sharing the same age, place of origin, chemical characteristics, and motion through space. From the perspective of observers on Earth, the Hyades Cluster appears in the constellation Taurus, where its brightest stars form a "V" shape along with the still-brighter Aldebaran. However, Aldebaran is unrelated to the Hyades, as it is located much closer to Earth and merely happens to lie along the same line of sight.

<span class="mw-page-title-main">Zeta Andromedae</span> Star system in the constellation Andromeda

Zeta Andromedae is a star system in the constellation Andromeda. It is approximately 189 light-years from Earth.

<span class="mw-page-title-main">HD 189733</span> Binary star system in the constellation Vulpecula

HD 189733, also catalogued as V452 Vulpeculae, is a binary star system 64.5 light-years away in the constellation of Vulpecula. The primary star is suspected to be an orange dwarf star, while the secondary star is a red dwarf star. Given that this system has the same visual magnitude as HD 209458, it promises much for the study of close transiting extrasolar planets. The star can be found with binoculars 0.3 degrees east of the Dumbbell Nebula (M27).

<span class="mw-page-title-main">AB Doradus</span> Pre-main sequence star system in the constellation Dorado

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.

<span class="mw-page-title-main">EQ Virginis</span> Star in the constellation Virgo

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.

<span class="mw-page-title-main">DT Virginis</span> Star in the constellation Virgo

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.

<span class="mw-page-title-main">FK Comae Berenices</span> Star in the constellation of Coma Berenices

FK Comae Berenices is a variable star that varies in apparent magnitude between 8.14 and 8.33 over a period of 2.4 days. It is the prototype for the FK Comae Berenices class of variable stars. The variability of FK Com stars may be caused by large, cool spots on the rotating surfaces of the stars. This star is thought to be the result of a recent binary merger, resulting in a high rate of both spin and magnetic activity.

HIP 70849 is a star with two non-stellar companions in the southern constellation Lupus. It is a 10th magnitude star, making it too faint to be visible to the naked eye. The system is located at a distance of 78.7 light-years from the Sun based on parallax measurements.

<span class="mw-page-title-main">111 Tauri</span> Wide binary star system in the constellation Taurus

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.

GJ 526 is a red dwarf star in the northern constellation of Boötes. It has an apparent visual magnitude of 8.5, which is too faint to be seen with the naked eye. Based upon an annual parallax shift of 0.184 arc seconds as measured by the Hipparcos satellite, this system is 17.7 light-years from Earth.

<span class="mw-page-title-main">XX Trianguli</span> Star system in the constellation Taurus

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.

<span class="mw-page-title-main">9 Ceti</span> Star in the constellation Cetus

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.

<span class="mw-page-title-main">HK Aquarii</span> Star in the constellation Aquarius

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.

<span class="mw-page-title-main">HD 111395</span> Star in the constellation Coma Berenices

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.

<span class="mw-page-title-main">V1794 Cygni</span> FK Comae Berenices variable in the constellation Cygnus

V1794 Cygni is a single variable star in the northern constellation Cygnus. It has the identifier HD 199178 from the Henry Draper Catalogue; V1794 Cygni is its variable star designation. With an apparent visual magnitude of 7.24, it's too dim to be visible with the naked eye but can be seen with binoculars. V1794 is located at a distance of 367 light-years (113 pc) based on parallax measurements, but is drifting closer to the Sun with a radial velocity of −31 km/s. It lies superimposed over a region of faint nebulosity to the west of the North American Nebula.

<span class="mw-page-title-main">HD 283572</span> Young star in constellation Taurus

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. Submillimeter Array (SMA) 1.3mm observations of HD 283572 detected an extreme brightening event with a radio luminosity of 8.3x1016erg/s/Hz that spanned 9 hours on January 17th 2022. Although HD 283572 was observed by the SMA on 8 separate nights, millimeter emission was detected on one night only, strongly suggesting stellar variability as a result of an extreme stellar flare.

<span class="mw-page-title-main">HD 165590</span> Triple star system in constellation Hercules

HD 165590 is a quintuple system dominated by the binary Algol variable star known as V772 Herculis. The system lies in the constellation of Hercules about 123 light years from the Sun, and is suspected to be a part of the Pleiades moving group.

<span class="mw-page-title-main">LQ Hydrae</span> Star in the constellation Hydra

LQ Hydrae is a single variable star in the equatorial constellation of Hydra. It is sometimes identified as Gl 355 from the Gliese Catalogue; LQ Hydrae is the variable star designation, which is abbreviated LQ Hya. The brightness of the star ranges from an apparent visual magnitude of 7.79 down to 7.86, which is too faint to be readily visible to the naked eye. Based on parallax measurements, this star is located at a distance of 59.6 light years from the Sun. It is drifting further away with a radial velocity of 7.6 km/s.

<span class="mw-page-title-main">V471 Tauri</span> Variable star in the constellation Taurus

V471 Tauri is an eclipsing variable star in the constellation of Taurus. The star has a visual magnitude of 9 which makes it impossible to see with the naked eye. It is around 155 light-years away from the Solar System.

<span class="mw-page-title-main">LO Pegasi</span> Star in the constellation Pegasus

LO Pegasi is a single star in the northern constellation of Pegasus that has been the subject of numerous scientific studies. LO Pegasi, abbreviated LO Peg, is the variable star designation. It is too faint to be viewed with the naked eye, having an apparent visual magnitude that ranges from 9.04 down to 9.27. Based on parallax measurements, LO Peg is located at a distance of 79 light years from the Sun. It is a member of the young AB Doradus moving group, and is drifting closer with a radial velocity of −23 km/s.

References

  1. ↑ Strassmeier, K. G.; Bartus, J.; Cutispoto, G.; Rodono, M. (October 1997). "Starspot photometry with robotic telescopes: Continuous UBV and V(RI)_C photometry of 23 stars in 1991-1996". Astron. Astrophys. Suppl. Ser. 125 (1): 11–63. Bibcode:1997A&AS..125...11S. doi: 10.1051/aas:1997369 . Retrieved 29 June 2022.
  2. ↑ Oláh, K.; Kolláth, Z.; Strassmeier, K. G. (April 2000). "Multiperiodic light variations of active stars". Astronomy and Astrophysics. 356: 643–653. Bibcode:2000A&A...356..643O . Retrieved 29 June 2022.
  3. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  4. 1 2 3 "HD 283750". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 30 June 2021.
  5. 1 2 "V833 Tauri". International Variable Star Index. AAVSO . Retrieved 2022-06-29.
  6. 1 2 3 4 Naftilan, S. A.; Fairchild, K. (1993). "Abundance Analysis of the BY Draconis Variable, Hot Flare Star V833 Tauri". Publications of the Astronomical Society of the Pacific. 105: 565. doi:10.1086/133194. S2CID   121761886.
  7. 1 2 3 4 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  8. 1 2 3 Catalán, S.; Ribas, I.; Isern, J.; García-Berro, E. (2007), "WD0433+270: An old Hyades stream member or an Fe-core white dwarf?", Astronomy & Astrophysics, 477 (3): 901–906, arXiv: 0710.3999 , doi:10.1051/0004-6361:20078230, S2CID   1559222
  9. ↑ Scholz, R.-D.; Meusinger, H.; Jahreiß, H. (2018), "New nearby white dwarfs from Gaia DR1 TGAS and UCAC5/URAT", Astronomy & Astrophysics, 613: A26, arXiv: 1711.10778 , Bibcode:2018A&A...613A..26S, doi:10.1051/0004-6361/201731753, S2CID   59423840
  10. ↑ Toonen, S.; Hollands, M.; Gänsicke, B. T.; Boekholt, T. (2017), "The binarity of the local white dwarf population", Astronomy & Astrophysics, 602: A16, arXiv: 1703.06893 , Bibcode:2017A&A...602A..16T, doi:10.1051/0004-6361/201629978, S2CID   12367523
  11. 1 2 Oláh, K.; Strassmeier, K. G.; Kővári, Zs.; Guinan, E. F. (2001). "Time-series photometric spot modeling. IV. The multi-periodic K5Ve binary V833 Tauri". Astronomy & Astrophysics. 372: 119–129. Bibcode:2001A&A...372..119O. doi: 10.1051/0004-6361:20010362 .
  12. ↑ Frick, P.; Sokoloff, D.; Katsova, M. M.; Bondar', N. I.; Stepanov, R. (2020). "Wavelet analysis of the long-term activity of V833 Tau". Monthly Notices of the Royal Astronomical Society. 495 (4): 3788–3794. arXiv: 2005.11136 . doi: 10.1093/mnras/staa1458 .
  13. ↑ Bondar', N. I. (2017). "Photometric period and rotational brightness modulation of V833 Tau". Astronomy Reports. 61 (2): 130–137. Bibcode:2017ARep...61..130B. doi:10.1134/S1063772917010024. S2CID   126233507.
  14. ↑ Saar, S. H.; Martens, P. C. H.; Huovelin, J.; Linnaluoto, S. (1994). "Possible detection of a stellar flare-generated particle beam in polarized light". Astronomy and Astrophysics. 286: 194. Bibcode:1994A&A...286..194S.
  15. ↑ Bonavita, M.; Desidera, S.; Thalmann, C.; Janson, M.; Vigan, A.; Chauvin, G.; Lannier, J. (2016). "SPOTS: The Search for Planets Orbiting Two Stars II. First constraints on the frequency of sub-stellar companions on wide circumbinary orbits". Astronomy and Astrophysics. 593: 593. arXiv: 1605.03962 . Bibcode:2016A&A...593A..38B. doi:10.1051/0004-6361/201628231. S2CID   55950739.
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