HD 29697

Last updated
HD 29697
V834TauLightCurve.png
A light curve for V834 Tauri, plotted from Kepler data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Taurus
Right ascension 04h 41m 18.85634s [2]
Declination +20° 54′ 05.4456″ [2]
Apparent magnitude  (V)7.94 - 8.33 [3]
Characteristics
Spectral type K3 V [4]
U−B color index +0.94 [5]
B−V color index +1.09 [5]
Variable type BY Dra [6]
Astrometry
Radial velocity (Rv)+11 [7]  km/s
Proper motion (μ)RA: −232.38±1.05 [2]   mas/yr
Dec.: −254.28±0.69 [2]   mas/yr
Parallax (π)75.82 ± 1.14  mas [2]
Distance 43.0 ± 0.6  ly
(13.2 ± 0.2  pc)
Absolute magnitude  (MV)+7.49 [8]
Details
Mass 0.75 [9]   M☉
Radius 0.67 [9]   R☉
Luminosity 0.15 [9]   L☉
Surface gravity (log g)4.50 [6]   cgs
Temperature 4,454±11.4 [10]   K
Metallicity [Fe/H]0.01 [6]   dex
Rotational velocity (v sin i)9.73 [6]  km/s
Age 49±37 [9]   Myr
Other designations
V834 Tau, BD+20° 802, GJ  174, Gliese 174, HD  29697, HIP  21818, SAO  76708. [11]
Database references
SIMBAD data
ARICNS data

HD 29697 (Gliese 174, V834 Tauri) is a variable star of BY Draconis type in the constellation Taurus. It has an apparent magnitude around 8 and is approximately 43 ly away.

Description

HD 29697 is the Henry Draper Catalogue number of this star. It is also known by its designation in the Gliese Catalogue of Nearby Stars, Gliese 174, and its variable star designation V834 Tauri.

V834 Tauri is a BY Draconis variable with maximum and minimum apparent magnitudes of 7.94 and 8.33 respectively, [3] so it is never visible to the naked eye.

The star has been examined for indications of a circumstellar disk using the Spitzer Space Telescope, but no statistically-significant infrared excess was detected. [9]

Related Research Articles

Omicron Serpentis is a solitary star in the Serpens Cauda (tail) section of the equatorial constellation Serpens. Based upon an annual parallax shift of 18.83 mas as seen from Earth, it is located around 173 light years from the Sun. The star is visible to the naked eye with a base apparent visual magnitude of +4.26.

<span class="mw-page-title-main">Upsilon Ursae Majoris</span> Binary star in the constellation Ursa Major

Upsilon Ursae Majoris, Latinized from υ Ursae Majoris, is a binary star in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye with an apparent visual magnitude of +3.79. Based upon an annual parallax shift of 13.24 mas, it is located roughly 246 light-years from the Sun.

<span class="mw-page-title-main">Iota Canis Majoris</span> Variable star in the constellation Canis Major

Iota Canis Majoris, Latinized from ι Canis Majoris, is a solitary variable supergiant star in the southern constellation of Canis Major. It is visible to the naked eye with an apparent visual magnitude that varies between +4.36 and +4.40. The distance to this star is approximately 2,500 light years based on spectroscopic measurements. It is drifting further away with a radial velocity of +42 km/s.

<span class="mw-page-title-main">Gliese 105</span> Triple star system in the constellation Cetus

Gliese 105 is a triple star system in the constellation of Cetus. It is located relatively near the Sun at a distance of 23.6 light-years. Despite this, even the brightest component is barely visible with the unaided eye (see Bortle scale). No planets have yet been detected around any of the stars in this system.

<span class="mw-page-title-main">2 Centauri</span> Star in the constellation Centaurus

2 Centauri is a single star in the southern constellation of Centaurus, located approximately 183 light-years from Earth. It has the Bayer designation g Centauri; 2 Centauri is the Flamsteed designation. This object is visible to the naked eye as faint, red-hued star with an apparent visual magnitude of 4.19. It is moving away from the Earth with a heliocentric radial velocity of +41 km/s. The star is a member of the HR 1614 supercluster.

HD 1606 is a single star in the northern constellation of Andromeda, positioned a few degrees to the northeast of the bright star Alpheratz. It has a blue-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.87. Although it is suspected of variability, none has been conclusively found. The star is located at a distance of approximately 580 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +4 km/s. It has an absolute magnitude of −0.5.

<span class="mw-page-title-main">V538 Aurigae</span> Star in constellation Auriga

V538 Aurigae is a single star in the northern constellation of Auriga. With an apparent visual magnitude of 6.23, this star requires good dark sky conditions to view with the naked eye. It is located at a distance of 40.0 light-years (12.3 pc) from Sun based on parallax. The star is drifting further away with a radial velocity of 0.9 km/s. It is a member of the Local Association, and is most likely a thin disk star.

<span class="mw-page-title-main">Phi Draconis</span> Star in the constellation Draco

Phi Draconis is a fourth-magnitude variable star in the constellation Draco. It has the Flamsteed designation 43 Draconis. It is also a triple star system where the brightest component is a chemically peculiar Ap star.

<span class="mw-page-title-main">HD 190007</span> Star in the constellation Aquila

HD 190007, also known as Gliese 775, is a star with a close orbiting exoplanet in the constellation of Aquila. Parallax measurements by Gaia put the star at a distance of 41.5 light-years away from the Sun. It is drifting closer with a radial velocity of −30.3 km/s, and is predicted to come within 11.8 light-years in 375,000 years. The star has an absolute magnitude of 6.91, but at its present distance the apparent visual magnitude is 7.46, which is too faint to be viewed with the naked eye.

<span class="mw-page-title-main">Chi Ceti</span> Double star in the constellation Cetus

Chi Ceti , is the Bayer designation for a double star in the equatorial constellation of Cetus. They appear to be common proper motion companions, sharing a similar motion through space. The brighter component, HD 11171, is visible to the naked eye with an apparent visual magnitude of 4.66, while the fainter companion, HD 11131, is magnitude 6.75. Both lie at roughly the same distance, with the brighter component lying at an estimated distance of 75.6 light years from the Sun based upon an annual parallax shift of 43.13 mass.

<span class="mw-page-title-main">30 Cygni</span> Star in the constellation Cygnus

30 Cygni is a class A5III star in the constellation Cygnus. Its apparent magnitude is 4.83 and it is approximately 610 light years away based on parallax.

<span class="mw-page-title-main">Sigma Geminorum</span> Binary star system in the constellation Gemini

Sigma Geminorum is a binary star system in the constellation Gemini, just to the northwest of Pollux. It is visible to the naked eye with an apparent visual magnitude of 4.20. Its annual parallax shift of 26.08 mas indicates that it is located 125 light years from the Sun.

106 Herculis is a variable star in the northern constellation Hercules. It is visible to the naked eye as a faint, red-hued point of light with a baseline apparent visual magnitude of 4.96. Based on its parallax, it is estimated to lie 383 light-years away from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of -35 km/s.

Mu Muscae, Latinized from μ Muscae, is a solitary star in the southern constellation of Musca. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of around 4.75. Based upon an annual parallax shift of 7.21 mas as seen from Earth, it is located about 450 light years from the Sun. The star is drifting further away with a radial velocity of +37 km/s.

<span class="mw-page-title-main">QZ Puppis</span> Star in the constellation Puppis

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.

<span class="mw-page-title-main">R Leonis Minoris</span> Star in the constellation Leo Minor

R Leonis Minoris is a Mira variable type star in the constellation Leo Minor. It ranges between apparent magnitude 6.3 and 13.2, and spectral types M6.5e to M9.0e (Tc:), over a period of 372 days.

<span class="mw-page-title-main">Gliese 402</span> Star in the constellation Leo

Gliese 402 is a star located 22.7 light years from the Solar System. Located in the constellation of Leo, it is also known as Wolf 358 from its entry in Max Wolf's star catalogue. The stars nearest to Gliese 402 are Gliese 393, at 3.43 light years, Gliese 408, at 6.26 light years, and Gliese 382 at 6.66 light years.

<span class="mw-page-title-main">DS Crucis</span> Star in the constellation Crux

DS Crucis is a variable star near the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster. It is in the constellation Crux.

<span class="mw-page-title-main">6 Geminorum</span> Red supergiant star in the constellation Gemini

6 Geminorum is a variable star in the zodiac constellation of Gemini, located roughly 5,800 light years away from the Sun. It has the variable star designation BU Geminorum; 6 Geminorum is the Flamsteed designation. At its brightest this reddish hued star is barely visible to the naked eye but is readily visible with binoculars, found southeast of M 35, just to the south of WY Geminorum. It is moving further from the Earth with a heliocentric radial velocity of +27 km/s. The star is a member of the Gemini OB1 association.

<span class="mw-page-title-main">8 Draconis</span> White-hued chemically unusual star in the constellation Draco

8 Draconis, formally named Taiyi, is a single star in the northern circumpolar constellation of Draco. Based upon an annual parallax shift of 34.14 mas as seen from the Earth, the star is located approximately 96 light-years from the Sun. It is moving further away with a heliocentric radial velocity of +9 km/s, having come within 40.6 ly some 2.6 million years ago.

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 1 2 3 4 5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752 , Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID   18759600
  3. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. ↑ Montes, D.; et al. (2001), "Late-type members of young stellar kinematic groups - I. Single stars", Monthly Notices of the Royal Astronomical Society , 328 (1): 45–63, arXiv: astro-ph/0106537 , Bibcode:2001MNRAS.328...45M, doi: 10.1046/j.1365-8711.2001.04781.x , S2CID   55727428
  5. 1 2 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M
  6. 1 2 3 4 Mishenina, T. V.; et al. (November 2012), "Activity and the Li abundances in the FGK dwarfs", Astronomy & Astrophysics, 547: 8, arXiv: 1210.6843 , Bibcode:2012A&A...547A.106M, doi:10.1051/0004-6361/201118412, S2CID   119287319, A106
  7. ↑ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. Determination of Radial Velocities and Their Applications. Vol. 30. University of Toronto: International Astronomical Union. p. 57. Bibcode:1967IAUS...30...57E.
  8. ↑ Anderson, E; Francis, Ch (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID   119257644.
  9. 1 2 3 4 5 Plavchan, Peter; et al. (June 2009), "New Debris Disks Around Young, Low-Mass Stars Discovered with the Spitzer Space Telescope", The Astrophysical Journal, 698 (2): 1068–1094, arXiv: 0904.0819 , Bibcode:2009ApJ...698.1068P, doi:10.1088/0004-637X/698/2/1068, S2CID   51417657
  10. ↑ Kovtyukh, V. V.; et al. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios", Astronomy and Astrophysics , 411 (3): 559–564, arXiv: astro-ph/0308429 , Bibcode:2003A&A...411..559K, doi:10.1051/0004-6361:20031378, S2CID   18478960
  11. ↑ "HD 29697". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 6 February 2018.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.