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HD 25558 - Wikipedia

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HD 25558
Observation data Epoch J2000.0 Equinox J2000.0
A light curve for V1133 Tauri, plotted from TESS data.^[1] The 1.53 day period is marked in red.
Constellation	Taurus
Right ascension	04^h 03^m 44.60445^s^[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 (M_V)	−1.2^[6]

Details^[7]
Primary
Mass	4.6 `M`_☉
Radius	2.4^[a] `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^[a] `R`_☉
Luminosity	420+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

^ ^a ^b 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.

References

^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 16 January 2023.
^ ^a ^b ^c ^d ^e ^f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
^ ^a ^b Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". Vizier Online Data Catalog. 2237. Strasbourg astronomical Data Center. Bibcode:2002yCat.2237....0D. Retrieved 17 January 2023.
^ 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.
^ ^a ^b "V1133 Tau". International Variable Star Index. AAVSO. Retrieved 17 January 2023.
^ 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.
^ ^a ^b 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.
^ "40 Tau -- Double or Multiple Star". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-01-16.
^ 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.

Constellation of Taurus

Stars

Bayer	α (Aldebaran) β (Elnath) γ (Prima Hyadum) δ¹ (Secunda Hyadum) δ² δ³ ε (Ain) ζ (Tianguan) η (Alcyone) θ¹ θ² (Chamukuy) ι κ¹ κ² λ μ ν ξ ο π ρ σ¹ σ² τ υ φ χ ψ ω¹ ω²
Flamsteed	4 (s) 5 (f) 6 (t) 7 9 10 11 12 13 14 16 (Celaeno) 17 (Electra) 18 19 (Taygeta) 20 (Maia) 21 (Asterope) 22 (Asterope II) 23 (Merope) 24 26 27 (Atlas) 28 (Pleione) 29 (u) 30 (e) 31 32 33 36 37 (A¹) 39 (A²) 40 41 44 (p) 45 46 47 48 51 53 55 56 57 (h) 58 60 62 63 66 (r) 70 71 72 75 76 79 (b) 80 81 83 84 85 88 (d) 89 90 (c) 93 95 96 97 (i) 98 (k) 99 101 103 104 (m) 105 106 (l) 107 108 109 (n) 110 111 113 114 (o) 115 116 117 118 119 120 121 122 125 126 127 128 129 130 131 132 133 134 135 136 137 139 140 44 Eri 49 Eri
Variable	T Y Z RR RV RW RY RZ SU SV SZ TU UX UZ VY XX XZ AA AH BP CD CI CM CQ CT CU CW CY DD DF DG DH DI DL DM DN DO DQ DR DS EQ EU FN FS FU FV GG GI GK GV HK HL HU IK V410 V441 V471 V473 V479 V534 V624 V647 V650 V710 V711 V731 V766 V773 V774 V781 V807 V818 V819 V826 V827 V830 V833 V834 V836 V837 V892 V987 V1038 V1062 V1079 V1116 V1137 V1141 V1143 V1156 V1187 V1229 V1232 V1241 (WX Cas) V1298
HR	1023 1028 1039 1067 1085 1089 1102 1103 1110 1119 1137 1159 1172 1183 1185 1188 1201 1222 1224 1233 1237 1238 1253 1254 1257 1279 1280 1284 1295 1307 1310 1315 1349 1354 1358 1360 1370 1385 1400 1402 1403 1406 1413 1425 1427 1436 1442 1445 1446 1448 1455 1477 1480 1490 1512 1517 1554 1566 1575 1585 1633 1642 1741 1750 1755 1831 1847 1860 1878 1902 1921 1929 1954 1997 2013 2074
HD	21032 21585 23514 23712 24040 24368 24496 26292 27860 28086 28678 29627 29647 36112 37124 38263 38524 245134 285507
Other	2MASS J03552337+1133437 2MASS J04070752+1546457 2MASS J0441+2301 A0535+26 BD +24 692 Butterfly Star CoKu Tau/4 Elias 16 Elias 18 GD 71 Gliese 176 Haro 6-37 HBC 379 HH 30 HII 686 HII 1306 HII 1883 HII 3163 HP Tau/G2 Hubble I 4 HZ 9 IRAS 04239+2436 IRAS 04248+2612 IRAS 04325+2402 IRAS 04381+2540 K2-25 L1489 IRS L1527 L1551 IRS 5 L1521F-IRS MWC 480 PSR B0525+21 PSR B0540+23 PSR J0348+0432 PSR J0538+2813 Teide 1 TMR-1 TMC-1A WD 0346+246 WISE 0410+1502

Exoplanets	Aldebaran b ε Tauri b BD+20 594b HD 24040 b HD 37124 b c d Kojima-1Lb TOI-4603 b