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HD 9289

HD 9289
Location of HD 9289 (circled)
Observation data
Epoch J2000.0[1]      Equinox J2000.0[1]
Constellation Cetus
Right ascension 01h 31m 16.47427s
Declination −11° 07′ 07.9356″
Apparent magnitude (V) 9.38[2] (combined)
Characteristics
Evolutionary stage Main-sequence star
Spectral type A3V,[3] A3 SrEuCr[4]
Apparent magnitude (K) 9.08 ± 0.03 (A), 10.77 ± 0.05 (B)[5]
B−V color index 0.25[2]
J−H color index 0.086[6]
J−K color index 0.095[6]
Variable type Rapidly oscillating Ap star
Astrometry
Radial velocity (Rv)11.352±0.0017[7] km/s
Proper motion (μ) RA: -8.756[1] mas/yr
Dec.: −24.435[1] mas/yr
Parallax (π)3.2569 ± 0.1379 mas[1]
Distance1,000 ± 40 ly
(310 ± 10 pc)
Orbit[5]
PrimaryHD 9289 A
CompanionHD 9289 B
Semi-major axis (a)0.441±0.003″
Details
Luminosity8.7+1.5
−1.3[3] L☉
Surface gravity (log g)4.50±0.20[3] cgs
Temperature8710+410
−392,[3] 7750[8] K
Rotation8.660±0.006 d[8]
Rotational velocity (v sin i)10.50[9] km/s
Other designations
BW Ceti, BD−11° 286, Gaia DR2 2458519750738240768, Gaia DR3 2458519755033679360, HD 9289, SAO 147854, PPM 210286, TIC 136842396, TYC 5274-240-1, GSC 05274-00240, 2MASS J01311648-1107078[6]
Database references
SIMBADdata

HD 9289 is a white-hued variable star in the constellation of Cetus. It has the variable-star designation BW Ceti (abbreviated to BW Cet). With an apparent magnitude of 9.38, it is too faint to be observed by the naked eye from Earth. It is located at a distance of approximately 1,000 light-years (310 parsecs) according to Gaia EDR3 parallax measurements, and is moving away from the Solar System at a heliocentric radial velocity of 11.352 km/s.

Stellar properties

HD 9289 is an A-type main-sequence star with the spectral type A3 SrEuCr. The suffix indicates that the star shows strong spectral lines of strontium, europium, and chromium, characteristic of an Ap star. The star radiates roughly 8.7 times the luminosity of the Sun from its photosphere. It possesses a magnetic field with a strength of 2.0 kG,[10] which is 3,000–9,000 times stronger than Earth's magnetic field (0.22–0.67 G[11]).

Light curves for BW Ceti. The upper plot, adapted from Gruberbauer et al.[12] shows the short timescale variability, and the lower plot of TESS data[13] shows the longer timescale variability, with the rotation period marked in red.

The star was first classified as a rapidly oscillating Ap star (roAp) in 1993 by Kurtz et al. when it was found to pulsate at multiple periods, all clustered around 10.5 minutes (1585.06 μHz).[14] Additional observations confirmed the presence of rotational amplitude modulation, similar to that of the well-studied roAp star HR 1217.[15] In 2011, a new set of pulsation frequencies were discovered, the strongest of them being at 1585.936 μHz with an amplitude of 0.63 mmag. Few of them were consistent with the initial reports, however, which was explained by the fact that the measurements by Kurtz et al. were affected by aliasing that caused misidentifications, though an innate shift in the star's pulsation behavior could not be ruled out.[12]

In 2012, the rotational period of HD 9289 was constrained to 8.55±0.08 d through differential photometry observations.[16] This was revised slightly upward in 2021 to 8.660±0.006 d.[8]

Binary companion

In 2012, a previously undetected visual companion was discovered at a separation of 0.441 arcseconds to the east-northeast of HD 9289. The probability that the two stars are unrelated and aligned by chance is very low (2.16×10−4 %), therefore the pair are most certainly part of a wide binary system. The secondary star is about 1.70 magnitudes fainter than the primary when observed in the K band.[5]

References

  1. ^ a b c d 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.
  2. ^ a b Høg, E.; et al. (February 2000). "The Tycho-2 Catalogue of the 2.5 Million Brightest Stars". Astronomy and Astrophysics. 355 (1): L27–L30. Bibcode:2000A&A...355L..27H.
  3. ^ a b c d Shen, Dong-Xiang; et al. (1 October 2023). "Variability of Magnetic Hot Stars from the TESS Observations". The Astrophysical Journal. 955 (2): 123. arXiv:2308.15687. Bibcode:2023ApJ...955..123S. doi:10.3847/1538-4357/acf197. ISSN 0004-637X.
  4. ^ Renson, P.; Manfroid, J. (2009). "Catalogue of Ap, HgMn and Am stars". Astronomy & Astrophysics. 498 (3): 961–966. Bibcode:2009A&A...498..961R. doi:10.1051/0004-6361/200810788. ISSN 0004-6361.
  5. ^ a b c Schöller, M.; Correia, S.; Hubrig, S.; Kurtz, D. W. (2012). "Multiplicity of rapidly oscillating Ap stars". Astronomy & Astrophysics. 545: A38. arXiv:1208.0480. Bibcode:2012A&A...545A..38S. doi:10.1051/0004-6361/201118538. ISSN 0004-6361.
  6. ^ a b c "HD 9289". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 14 November 2024.
  7. ^ Soubiran, C.; et al. (2018). "Gaia Data Release 2: The catalogue of radial velocity standard stars". Astronomy & Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. ISSN 0004-6361.
  8. ^ a b c Holdsworth, D L; et al. (13 July 2021). "TESS cycle 1 observations of roAp stars with 2-min cadence data". Monthly Notices of the Royal Astronomical Society. 506 (1): 1073–1110. arXiv:2105.13274. doi:10.1093/mnras/stab1578. ISSN 0035-8711.
  9. ^ Joshi, S.; Martinez, P.; Chowdhury, S.; Chakradhari, N. K.; Joshi, Y. C.; van Heerden, P.; Medupe, T.; Kumar, Y. B.; Kuhn, R. B. (2016). "The Nainital-Cape Survey: IV. A search for pulsational variability in 108 chemically peculiar stars⋆". Astronomy & Astrophysics. 590: A116. arXiv:1603.03517. Bibcode:2016A&A...590A.116J. doi:10.1051/0004-6361/201527242. ISSN 0004-6361.Record for this source at VizieR.
  10. ^ Ryabchikova, T.; Sachkov, M.; Kochukhov, O.; Lyashko, D. (2007). "Pulsation tomography of rapidly oscillating Ap stars: Resolving the third dimension in peculiar pulsating stellar atmospheres". Astronomy & Astrophysics. 473 (3): 907–922. arXiv:0708.0289. Bibcode:2007A&A...473..907R. doi:10.1051/0004-6361:20077230. ISSN 0004-6361.
  11. ^ "An Overview of the Earth's Magnetic Field". www.geomag.bgs.ac.uk. Retrieved 2 March 2024.
  12. ^ a b Gruberbauer, M.; Huber, D.; Kuschnig, R.; Weiss, W. W.; Guenther, D. B.; Matthews, J. M.; Moffat, A. F. J.; Rowe, J. F.; Rucinski, S. M.; Sasselov, D.; Fischer, M. (2011). "MOST observations of the roAp stars HD 9289, HD 99563, and HD 134214". Astronomy & Astrophysics. 530: A135. arXiv:1104.2256. Bibcode:2011A&A...530A.135G. doi:10.1051/0004-6361/201116736. ISSN 0004-6361.
  13. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 16 November 2024.
  14. ^ Kurtz, D. W.; Martinez, P. (27 December 1993). "Discovery of 10.5-minute Oscillations in the Ap SrEu Star HD 9289". Information Bulletin on Variable Stars. 3966 (3966). Konkoly Observatory, Budapest: International Astronomical Union: 1. Bibcode:1993IBVS.3966....1K.
  15. ^ Kurtz, D. W.; Martinez, P.; Tripe, P. (15 November 1994). "HD 9289: a new rapidly oscillating Ap star similar to the well-studied, multiperiodic roAp star HR 1217". Monthly Notices of the Royal Astronomical Society. 271 (2): 421–426. doi:10.1093/mnras/271.2.421. ISSN 0035-8711.
  16. ^ van Heerden, P.; Martinez, P.; Kilkenny, D. (21 October 2012). "Determination of the rotation periods for the roAp stars HD 9289 and HD 190290 and non-detection of rotational amplitude modulation in the roAp stars HD 75425 and HD 217522: Rotation periods of selected Ap stars". Monthly Notices of the Royal Astronomical Society. 426 (2): 969–974. doi:10.1111/j.1365-2966.2012.21814.x.
Quelle: https://en.wikipedia.org/wiki/HD_9289