Jump to content

PW Telescopii

From Wikipedia, the free encyclopedia
PW Telescopii

A light curve for PW Telescopii, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Telescopium
Right ascension 19h 33m 21.62239s[2]
Declination −45° 16′ 18.3946″[2]
Apparent magnitude (V) 5.58±0.01[3]
Characteristics
Spectral type A0 Vp (SrCr)[4]
B−V color index −0.04[5]
Variable type α2 CVn[6]
Astrometry
Radial velocity (Rv)−10.3±2.7[7] km/s
Proper motion (μ) RA: −17.146 mas/yr[2]
Dec.: −24.625 mas/yr[2]
Parallax (π)8.2532 ± 0.1701 mas[2]
Distance395 ± 8 ly
(121 ± 2 pc)
Absolute magnitude (MV)+0.17[8]
Details
Mass2.79±0.14[9] M☉
Radius3.41[10] R☉
Luminosity100+26
−21[9] L☉
Surface gravity (log g)3.68[11] cgs
Temperature10,070[12] K
Metallicity [Fe/H]+1.09[13] dex
Rotational velocity (v sin i)55±6[14] km/s
Age363[15] Myr
Other designations
63 G. Telescopii[16], PW Tel, CD−45°13296, CPD−45°9740, FK5 3558, GC 29681, HD 183806, HIP 96178, HR 7416, SAO 229741[17]
Database references
SIMBADdata

PW Telescopii, also known as HD 183806 or simply PW Tel, is a solitary variable star[18] located in the southern constellation Telescopium. It has an average apparent magnitude of 5.58,[3] making it faintly visible to the naked eye. Based on parallax measurements from the Gaia satellite, the star is estimated to be 395 light years distant.[2] It appears to be approaching the Solar System with a heliocentric radial velocity of −10 km/s.[7] The value is somewhat constrained, having an uncertainty of 26%. At its current distance, PW Tel's brightness is diminished by 0.05 magnitudes due to interstellar dust.[19]

PW Tel was first noticed to vary in brightness in observations taken in 1978 by Pierre Renson.[20] The star was confirmed to be variable and was given the variable star designation PW Telescopii in 1981. Further observations by Jean Manfroid in 1985 improved earlier data, including the star's period.[21] PW Tel is an α2 CVn variable[6] that has an amplitude of 0.011 magnitudes within the visual passband and a period of 2.92 days.[22]

With a stellar classification of A0 Vp (SrCr), PW Tel is a chemically peculiar A-type main-sequence star.[4] It has been recognised as an Ap star, as indicated by the "p" suffix, since the early 20th century, and it shows an overabundance of strontium and chromium in its spectrum. The abundance of some metals in the spectrum is several hundred times higher than in the Sun and it has an overall metallicity of [Fe/H] = 1.09, but this only reflects levels of those elements in the photosphere, not the whole star.[13] Like most such stars it spins relatively slowly, with a projected rotational velocity of 55 km/s.[14]

With 2.8 times the mass of the Sun[9] and 3.4 times its radius,[10] PV Tel radiates 100 times the luminosity of the Sun[9] from its photosphere at an effective temperature of 10,070 K,[12] giving it a bluish-white hue. PW Tel is metal enriched, having an iron abundance over 10 times that of the Sun.[23]

References

[edit]
  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e 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.
  3. ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN 0004-6361.
  4. ^ a b Abt, Helmut A.; Morrell, Nidia I. (July 1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". The Astrophysical Journal Supplement Series. 99: 135. Bibcode:1995ApJS...99..135A. doi:10.1086/192182. ISSN 0067-0049.
  5. ^ Corben, P. M. (April 1971). "Photoelectric Magnitudes and Colours for Bright Southern Stars". Monthly Notes of the Astronomical Society of South Africa. 30 (4): 37. Bibcode:1971MNSSA..30...37C. ISSN 0024-8266.
  6. ^ a b Samus’, N. N.; Goranskii, V. P.; Durlevich, O. V.; Zharova, A. V.; Kazarovets, E. V.; Kireeva, N. N.; Pastukhova, E. N.; Williams, D. B.; Hazen, M. L. (July 2003). "An electronic version of the second volume of the General Catalogue of Variable Stars with improved coordinates". Astronomy Letters. 29 (7): 468–479. Bibcode:2003AstL...29..468S. doi:10.1134/1.1589864. eISSN 1562-6873. ISSN 1063-7737. S2CID 16299532.
  7. ^ a b Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. eISSN 1562-6873. ISSN 1063-7737. S2CID 119231169.
  8. ^ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 119257644.
  9. ^ a b c d Kochukhov, O.; Bagnulo, S. (10 April 2006). "Evolutionary state of magnetic chemically peculiar stars". Astronomy and Astrophysics. 450 (2): 763–775. arXiv:astro-ph/0601461. Bibcode:2006A&A...450..763K. doi:10.1051/0004-6361:20054596. eISSN 1432-0746. ISSN 0004-6361.
  10. ^ a b Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics. 657: A7. arXiv:2109.10912. Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. eISSN 1432-0746. ISSN 0004-6361.
  11. ^ Ghazaryan, S; Alecian, G; Hakobyan, A A (19 July 2018). "New catalogue of chemically peculiar stars, and statistical analysis". Monthly Notices of the Royal Astronomical Society. 480 (3): 2953–2962. arXiv:1807.06902. Bibcode:2018MNRAS.480.2953G. doi:10.1093/mnras/sty1912. eISSN 1365-2966. ISSN 0035-8711.
  12. ^ a b Ryabchikova, T. A. (June 2005). "Temperature behavior of elemental abundances in the atmospheres of magnetic peculiar stars". Astronomy Letters. 31 (6): 388–397. Bibcode:2005AstL...31..388R. doi:10.1134/1.1940111. eISSN 1562-6873. ISSN 1063-7737. S2CID 123429273.
  13. ^ a b Ghazaryan, S.; Alecian, G.; Hakobyan, A. A. (2018). "New catalogue of chemically peculiar stars, and statistical analysis". Monthly Notices of the Royal Astronomical Society. 480 (3): 2953–2962. arXiv:1807.06902. Bibcode:2018MNRAS.480.2953G. doi:10.1093/mnras/sty1912. S2CID 119062018.
  14. ^ a b Netopil, Martin; Paunzen, Ernst; Hümmerich, Stefan; Bernhard, Klaus (17 March 2017). "An investigation of the rotational properties of magnetic chemically peculiar stars". Monthly Notices of the Royal Astronomical Society. 468 (3): 2745–2756. arXiv:1703.05218. Bibcode:2017MNRAS.468.2745N. doi:10.1093/mnras/stx674. eISSN 1365-2966. ISSN 0035-8711.
  15. ^ Glagolevskij, Yu. V. (January 2019). "On Properties of Main Sequence Magnetic Stars". Astrophysical Bulletin. 74 (1): 66–79. Bibcode:2019AstBu..74...66G. doi:10.1134/S1990341319010073. eISSN 1990-3421. ISSN 1990-3413. S2CID 149900274.
  16. ^ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  17. ^ "PW Telescopii". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved November 22, 2022.
  18. ^ Eggleton, P. P.; Tokovinin, A. A. (11 September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. eISSN 1365-2966. ISSN 0035-8711.
  19. ^ Chen, P. S.; Liu, J. Y.; Shan, H. G. (18 April 2017). "A New Photometric Study of Ap and Am Stars in the Infrared". The Astronomical Journal. 153 (5): 218. Bibcode:2017AJ....153..218C. doi:10.3847/1538-3881/aa679a. eISSN 1538-3881.
  20. ^ Renson, P. (March 1978). "Nouvelle Recherche de Periodes D'etoiles Ap Observees a l'ESO - I". Information Bulletin on Variable Stars. 1391: 1. Bibcode:1978IBVS.1391....1R. ISSN 0374-0676.
  21. ^ Manfroid, J.; Mathys, G. (March 1985). "New period determinations for variable CP stars". Astronomy and Astrophysics Supplement Series. 59: 429–432. Bibcode:1985A&AS...59..429M. ISSN 0365-0138.
  22. ^ Samus’, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (January 2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. eISSN 1562-6881. ISSN 1063-7729. S2CID 125853869.
  23. ^ Kearsley, A. J.; Wegner, G. (1 February 1978). "Atmospheric analyses of southern peculiar A stars". Monthly Notices of the Royal Astronomical Society. 182 (2): 117–125. Bibcode:1978MNRAS.182..117K. doi:10.1093/mnras/182.2.117. eISSN 1365-2966. ISSN 0035-8711.
Retrieved from "http://en.wiki.x.io/w/index.php?title=PW_Telescopii&oldid=1235286505"