HD 25558

Last updated
HD 25558
V1133TauLightCurve.png
A light curve for V1133 Tauri, plotted from TESS data. [1] The 1.53 day period is marked in red.
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Taurus
Right ascension 04h 03m 44.60445s [2]
Declination +05° 26′ 08.2258″ [2]
Apparent magnitude  (V)+5.33 [3]
Characteristics
Spectral type B3V [4]
Variable type Slowly pulsating B-type star [5]
Astrometry
Proper motion (μ)RA: 1.271±0.275 [2]   mas/yr
Dec.: −7.216±0.201 [2]   mas/yr
Parallax (π)4.5161 ± 0.2637  mas [2]
Distance 720 ± 40  ly
(220 ± 10  pc)
Absolute magnitude  (MV)−1.2 [6]
Details [7]
Primary
Mass 4.6  M☉
Radius 2.4 [lower-alpha 1]   R☉
Luminosity 560+530
−270  L☉
Surface gravity (log g)4.2±0.2  cgs
Temperature 16,850±800  K
Metallicity [Fe/H]−0.3  dex
Rotation 5.9±2  d
Rotational velocity (v sin i)21.5±1.5 km/s
Secondary
Mass 4.2  M☉
Radius 2.9 [lower-alpha 1]   R☉
Luminosity420+540
−230  L☉
Surface gravity (log g)4.25±0.25  cgs
Temperature 16,250±1,000  K
Metallicity [Fe/H]−0.3  dex
Rotation 1.2±0.6  d
Rotational velocity (v sin i)35±4 km/s
Age 40-55  Myr
Other designations
40 Tauri, V1133 Tau, BD+05 584, HIP  18957, HR  1253, SAO  111585 [8]
Database references
SIMBAD data

HD 25558, also known as V1133 Tauri and by its Flamsteed designation 40 Tauri, is a star located about 700 light years from the Earth, in the constellation Taurus. [2] Its apparent magnitude is about 5.3, [3] making it faintly visible to the naked eye of an observer far from city lights. It is a variable star, ranging in brightness from Hipparcos magnitude 5.28 to 5.32 over a period of 1.53232423 days. [5]

In 1998, HD 25558 was discovered to be a variable star by Christoffel Waelkens et al. who analyzed the Hipparcos photometric data for hundreds of stars, and classified HD 25558 as a slowly pulsating B star with a period of 1.53 days. [9]

Beginning in 2008, HD 25558 was the subject of an observing campaign by Ádám Sódor et al. who gathered data collected from 17 observatories on the ground and in space. This star was chosen for the project because it is relatively bright, located near the celestial equator (and thus observable from almost anywhere on Earth), and the slow rotation indicated in earlier studies would simplify the interpretation of spectra. The investigators concluded that HD 25558 is a spectroscopic binary with a period of about 8.9 years, but not enough data was available to derive a full description of the orbit. Both components of the binary show detectable stellar pulsations. The primary star rotates with a period of about 6 days, and the secondary rotates in just 1.2 days. The primary has no detectable magnetic field, but the secondary's field strength is at least a few hundred gauss. The dominant 1.53 day pulsation period arises from the primary star and those pulsations were coherent over the 20 year period spanned by the data used in the study. [7]

Notes

  1. 1 2 The paper derives the period from the rotational velocity and the radius, but does not show the radius. The radius found can be calculated from the period and equatorial rotational velocity.

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References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 16 January 2023.
  2. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . Gaia DR3 record for this source at VizieR.
  3. 1 2 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". Vizier Online Data Catalog. Strasbourg astronomical Data Center. Bibcode:2002yCat.2237....0D . Retrieved 17 January 2023.
  4. ↑ Lesh, Janet Rountree (December 1968). "The Kinematics of the Gould Belt: an Expanding Group?". Astrophysical Journal Supplement. 17: 371. Bibcode:1968ApJS...17..371L. doi: 10.1086/190179 .
  5. 1 2 "V1133 Tau". International Variable Star Index. AAVSO. Retrieved 17 January 2023.
  6. ↑ Shultz, M. E.; et al. (May 2019). "The magnetic early B-type Stars II: stellar atmospheric parameters in the era of Gaia". Monthly Notices of the Royal Astronomical Society. 485 (2): 1508–1527. arXiv: 1902.02713 . Bibcode:2019MNRAS.485.1508S. doi:10.1093/mnras/stz416.
  7. 1 2 Sódor, Á.; De Cat, P.; Wright, D. J.; Neiner, C.; Briquet, M.; Lampens, P.; Dukes, R. J.; Henry, G. W.; Williamson, M. H.; Brunsden, E.; Pollard, K. R.; Cottrell, P. L.; Maisonneuve, F.; Kilmartin, P. M.; Matthews, J.; Kallinger, T.; Beck, P. G.; Kambe, E.; Engelbrecht, C. A.; Czanik, R. J.; Yang, S.; Hashimoto, O.; Honda, S.; Fu, J. N.; Castanheira, B.; Lehmann, H.; Bognár, Zs.; Behara, N.; Scaringi, S.; Van Winckel, H.; Menu, J.; Lobel, A.; Mathias, P.; Saesen, S.; Vučković, M.; the MiMeS collaboration (March 2014). "Extensive study of HD 25558, a long-period double-lined binary with two SPB components". Monthly Notices of the Royal Astronomical Society. 438 (4): 3535–3556. arXiv: 1312.6307 . Bibcode:2014MNRAS.438.3535S. doi: 10.1093/mnras/stt2466 .
  8. ↑ "40 Tau -- Double or Multiple Star". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-01-16.
  9. ↑ Waelkens, C.; Aerts, C.; Kestens, E.; Grenon, M.; Eyer, L. (February 1998). "Study of an unbiased sample of B stars observed with Hipparcos: the discovery of a large amount of new slowly pulsating B stars". Astronomy and Astrophysics. 330: 215–221. Bibcode:1998A&A...330..215W.
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