Movatterモバイル変換

[0]ホーム
URL:

Jump to content
WikipediaThe Free Encyclopedia
Search

TT Cygni

From Wikipedia, the free encyclopedia
Star in the constellation Cygnus
TT Cygni

Alight curve for TT Cygni, plotted fromHipparcos data[1]
Observation data
Epoch J2000.0      Equinox J2000.0
ConstellationCygnus
Right ascension19h 40m 57.01599s[2]
Declination+32° 37′ 05.7555″[2]
Apparent magnitude (V)7.26 - 8.0[3]
Characteristics
Evolutionary stageAGB[4]
Spectral typeC5,4e(N3e)[3]
B−Vcolor index+2.917±0.073[5]
Variable typeSRb[6]
Astrometry
Radial velocity (Rv)−49.0±3.1[5] km/s
Proper motion (μ)RA: −5.178[2]mas/yr
Dec.: −1.832[2]mas/yr
Parallax (π)1.4908±0.0368 mas[2]
Distance2,190 ± 50 ly
(670 ± 20 pc)
Absolute magnitude (MV)−1.297 (var.)[7]
Details
Mass3.4[8] M☉
Radius166[9] R☉
Luminosity2,735[10] L☉
Surface gravity (log g)−0.4[10] cgs
Temperature3,200[10] K
Metallicity[Fe/H]−9.49[8] dex
Other designations
TT Cyg,BD+32°3522,HD 186047,HIP 96836,SAO 68688[11]
Database references
SIMBADdata

TT Cygni is acarbon star located 561 parsecs (1,830 ly) away in the northernconstellation ofCygnus. It is classified as asemiregular variable of subtype SRb that ranges in brightness from magnitude 7.26 down to 8.0 with a period of 118 days.[3] This object is called a carbon star because it has a high ratio ofcarbon tooxygen in its surface layers. The carbon was produced byhelium fusion,dredged up from inside the star by deep convection triggered by a flash from the helium shell.

In 1898 it was announced that Louisa Dennison Wells had discovered that the star, then known as BD +32°3522, is avariable star.[12] It was listed with itsvariable star designation, TT Cygni, inAnnie Jump Cannon's 1907 workSecond Catalog of Variable Stars.[13]

A thin spherical shell around the star, about half a light year across, was emitted 7,000 years ago.[14] It was first detected from itscarbon monoxide emission and has a mass around four thousandths M☉, of which about a tenth is dust. The dust is thought to be mostlyamorphous carbon.[10]

References

[edit]
  1. ^"Hipparcos Tools Interactive Data Access".Hipparcos. ESA. Retrieved8 December 2021.
  2. ^abcdeBrown, A. G. A.; et al. (Gaia collaboration) (August 2018)."Gaia Data Release 2: Summary of the contents and survey properties".Astronomy & Astrophysics.616. A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source atVizieR.
  3. ^abc"TT Cygni".International Variable Star Index.AAVSO. Retrieved2021-02-04.
  4. ^Maercker, M.; De Beck, E.; Khouri, T.; Vlemmings, W. H. T.; Gustafsson, J.; Olofsson, H.; Tafoya, D.; Kerschbaum, F.; Lindqvist, M. (2024). "Probing the dynamical and kinematical structures of detached shells around AGB stars".Astronomy and Astrophysics.687: A112.arXiv:2405.01222.Bibcode:2024A&A...687A.112M.doi:10.1051/0004-6361/202449643.
  5. ^abAnderson, 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.
  6. ^Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars".Astronomy Reports. 5.1.61 (1):80–88.Bibcode:2017ARep...61...80S.doi:10.1134/S1063772917010085.S2CID 125853869.
  7. ^Gontcharov, G. A. (2011). "The red giant branch in the Tycho-2 catalogue".Astronomy Letters.37 (10):707–717.arXiv:1607.00557.Bibcode:2011AstL...37..707G.doi:10.1134/S1063773711090040.S2CID 119272127.
  8. ^abKhalatyan, A.; Anders, F.; Chiappini, C.; Queiroz, A. B. A.; Nepal, S.; Dal Ponte, M.; Jordi, C.; Guiglion, G.; Valentini, M.; Torralba Elipe, G.; Steinmetz, M.; Pantaleoni-González, M.; Malhotra, S.; Jiménez-Arranz, Ó.; Enke, H.; Casamiquela, L.; Ardèvol, J. (2024). "Transferring spectroscopic stellar labels to 217 million Gaia DR3 XP stars with SHBoost".Astronomy and Astrophysics.691: A98.arXiv:2407.06963.Bibcode:2024A&A...691A..98K.doi:10.1051/0004-6361/202451427.
  9. ^McDonald, I.; Zijlstra, A. A.; Watson, R. A. (2017)."Fundamental parameters and infrared excesses of Tycho–Gaia stars".Monthly Notices of the Royal Astronomical Society.471 (1):770–791.arXiv:1706.02208.Bibcode:2017MNRAS.471..770M.doi:10.1093/mnras/stx1433.
  10. ^abcdGroenewegen, M. A. T. (2012)."An extension of the DUSTY radiative transfer code and an application to OH 26.5 and TT Cygni".Astronomy and Astrophysics.543: A36.Bibcode:2012A&A...543A..36G.doi:10.1051/0004-6361/201218965.
  11. ^"TT Cyg".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2021-02-03.
  12. ^Pickering, E. C.; Bailey, S. I.; Fleming, W. P.; Leland, E. F.; Wells, L. D. (March 1898). "Variable star clusters. New variable stars".Astrophysical Journal.7:208–211.Bibcode:1898ApJ.....7..208P.doi:10.1086/140457.
  13. ^Cannon, Annie J. (1907). "Second catalogue of variable stars".Annals of Harvard College Observatory.55:1–94.Bibcode:1907AnHar..55....1C.
  14. ^Olofsson, H.; et al. (January 2000). "A high-resolution study of episodic mass loss from the carbon star TT Cygni".Astronomy and Astrophysics.353:583–597.Bibcode:2000A&A...353..583O.
Stars
Bayer
Flamsteed
Variable
HR
HD
Gliese
Kepler
WR
Other
Star
clusters
Association
Open
Molecular
clouds
Nebulae
Dark
H II
Planetary
WR
SNR
Galaxies
NGC
Other
Exoplanets
Kepler
Other
Exomoons
Kepler
Retrieved from "https://en.wikipedia.org/w/index.php?title=TT_Cygni&oldid=1289905209"
Categories:
Hidden categories:
[8]ページ先頭
©2009-2026 Movatter.jp