V Hydrae

From Wikipedia, the free encyclopedia
Jump to: navigation, search
V Hydrae
Hydra constellation map.svg
Red circle.svg

Location of V Hydrae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Hydra
Right ascension 10h 51m 37.25661s[1]
Declination −21° 15′ 00.3245″[1]
Apparent magnitude (V) 6.0 - 12.3[2]
Characteristics
Spectral type C6,3e-C7,5e(N6e)[3]
B−V color index +5.43[4]
Variable type SRa[3]
Astrometry
Radial velocity (Rv) −14.80[5] km/s
Proper motion (μ) RA: −11.02 ± 1.14[1] mas/yr
Dec.: 2.29 ± 1.16[1] mas/yr
Parallax (π) 1.44 ± 1.41[1] mas
Distance approx. 2,000 ly
(approx. 700 pc)
Absolute magnitude (MV) −3.5 to +1.8[6]
Orbit[7]
Period (P) 8.5 yr
Eccentricity (e) ≥0.6
Details
A
Mass 1.0[8] M
Radius 430[7] R
Luminosity 7,850[8] L
Surface gravity (log g) −0.5[8] cgs
Temperature 2,650[8] K
Rotational velocity (v sin i) 11 - 14[8] km/s
B
Mass <1[7] M
Other designations
V Hya, BD−20°3283, HIP 53085, 2MASS J10513724-2115002, IRAS 10491-2059, WDS J10516-2115
Database references
SIMBAD data

V Hydrae (V Hya) is a carbon star in the constellation Hydra.

Variability[edit]

Artist's illustration of plasma ejections from V Hydrae.

V Hydrae is a semiregular variable star of type SRa, sometimes considered to be a Mira variable. It pulsates with a period of 530 days and a brightness range of 1-2 magnitudes, but also shows deep fades at intervals of about 6,160 days when it may drop below magnitude 12.[2][9]

Evolutionary stage[edit]

V Hydrae is a carbon star, an asymptotic giant branch (AGB) star that has dredged up sufficient material from its interior to have more carbon in its atmosphere than oxygen. The rate of mass loss from V Hydrae indicates that it is almost at the end of the AGB stage and about to lose its atmosphere completely and form a planetary nebula. It is sometimes considered to be a post-AGB object.[10]

Companions[edit]

V Hydrae has a visible binary companion 46" distant. It is a magnitude 11.5 K0 giant.[6]

V Hydrae also has an unseen companion in an 8.5 year orbit, inferred by its ultraviolet excess and eruptions associated with the periastron passage.[11][7] It has been suggested that the steep drops in brightness every 17 years or so are caused by obscuration by a cloud associated with the companion passing in front of the giant star.[11]

Bullets[edit]

V Hydrae has high-speed outflows of material collimated into jets, and also a disk of material around the star. Since the star itself is considered to be at the end of the Asymptotic Giant Branch phase of evolution and starting to generate a planetary nebula, the mechanism for the ejection of this material can give key insights to the formation of planetary nebulae. The ejections have been modelled as bullets of material fired out each time the compact companion passes close to the extended giant star during a highly eccentric orbit. The bullets are ejected in opposite directions in different orbits due to a flip-flop of the ejection mechanism.[7]

References[edit]

  1. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. 
  2. ^ a b Watson, Christopher (4 January 2010). "V Hydrae". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 2016-10-12. 
  3. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S. 
  4. ^ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D. 
  5. ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. 
  6. ^ a b Gordon, Courtney P. (1968). "The Absolute Magnitudes of Carbon Stars". Publications of the Astronomical Society of the Pacific. 80: 597. Bibcode:1968PASP...80..597G. doi:10.1086/128694. 
  7. ^ a b c d e Sahai, R.; Scibelli, S.; Morris, M. R. (2016). "High-speed Bullet Ejections during the AGB-to-Planetary Nebula Transition: HST Observations of the Carbon Star, V Hydrae". The Astrophysical Journal. 827 (2): 92. arXiv:1605.06728Freely accessible. Bibcode:2016ApJ...827...92S. doi:10.3847/0004-637X/827/2/92. 
  8. ^ a b c d e Zhao-Geisler, R.; Quirrenbach, A.; Köhler, R.; Lopez, B. (2012). "Dust and molecular shells in asymptotic giant branch stars". Astronomy & Astrophysics. 545: A56. arXiv:1207.3767Freely accessible. Bibcode:2012A&A...545A..56Z. doi:10.1051/0004-6361/201118150. 
  9. ^ Olivier, Enrico A.; Whitelock, Patricia; Marang, Fred (2001). "Dust-enshrouded asymptotic giant branch stars in the solar neighbourhood". Monthly Notices of the Royal Astronomical Society. 326 (2): 490. arXiv:astro-ph/0103294Freely accessible. Bibcode:2001MNRAS.326..490O. doi:10.1046/j.1365-8711.2001.04511.x. 
  10. ^ Knapp, G. R.; Crosas, M.; Young, K.; Ivezić, Željko (2000). "Atomic Carbon in the Envelopes of Carbon‐rich Post–Asymptotic Giant Branch Stars". The Astrophysical Journal. 534: 324. doi:10.1086/308731. 
  11. ^ a b Sahai, R.; Findeisen, K.; Gil De Paz, A.; Sánchez Contreras, C. (2008). "Binarity in Cool Asymptotic Giant Branch Stars: A GALEX Search for Ultraviolet Excesses". The Astrophysical Journal. 689 (2): 1274–1278. Bibcode:2008ApJ...689.1274S. doi:10.1086/592559.