Z Chamaeleontis
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Chamaeleon |
| Right ascension | 08h 07m 27.7518s |
| Declination | −76° 32′ 00.665″ |
| Apparent magnitude (V) | 11.5 - 16.2 |
| Characteristics | |
| Spectral type | DA? + M5.5e |
| Variable type | SU UMa + Algol |
| Astrometry | |
| Radial velocity (Rv) | −20 km/s |
| Proper motion (μ) | RA: −33.650 mas/yr Dec.: +56.883 mas/yr |
| Parallax (π) | 8.2805±0.074 mas |
| Distance | 394 ± 4 ly (121 ± 1 pc) |
| Orbit | |
| Primary | white dwarf |
| Secondary | red dwarf |
| Period (P) | 0.0744992631(3) days (1.79 h) |
| Semi-major axis (a) | 0.734±0.005 R☉ |
| Eccentricity (e) | 0 |
| Inclination (i) | 80.44±0.11° |
| Semi-amplitude (K1) (primary) | 78.4+1.1 −1.8 km/s |
| Semi-amplitude (K2) (secondary) | 413.2+2.5 −2.0 km/s |
| Details | |
| white dwarf | |
| Mass | 0.803±0.014 M☉ |
| Radius | 0.01046±0.00017 R☉ |
| Surface gravity (log g) | 8.304±0.016 cgs |
| Temperature | 16,300±1,400 K |
| red dwarf | |
| Mass | 0.152±0.005 M☉ |
| Radius | 0.1820±0.0020 R☉ |
| Other designations | |
| Z Cha, 2E 1942, SBC9 505, CSV 1244, 2MASS J08072774-7632006, SON 4893, 2E 0808.8-7622, 1RXS J080728.8-763157, AAVSO 0809-76 | |
| Database references | |
| SIMBAD | data |
Z Chamaeleontis (abbreviated Z Cha) is a dwarf nova variable star system approximately 394 light-years away from the Sun, where two stars orbit each other every 1.78 hours. The system comprises an eclipsing white dwarf and red dwarf and possibly a yet unconfirmed third low-mass substellar companion.
Z Chamaeleontis was discovered in 1904, during the work required to produce the Astrographic Catalogue. By 1905 a period of variability had been derived. in 1969, George S. Mumford discovered that in addition to being a dwarf nova, the star is an eclipsing variable.
Substellar companion
Dai et al. (2009) invoke the presence of a third object to explain orbital period variations with an apparent periodicity of roughly 28 years. The third body could yield a minimum mass 20 times greater than Jupiter and be located 9.9 Astronomical Units away from the dwarf nova, being likely a low-mass brown dwarf.
_Z_Chamaeleontis_Star_system.png)
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | ≥20 MJ | 9.9 | 28 | ≤0.2 | — | — |
See also
References
- ↑ Wood, Janet; Horne, Keith; Berriman, Graham; Wade, R.; O'Donoghue, D.; Warner, B. (April 1986). "High-speed photometry of the dwarf nova Z Cha in quiescence". Monthly Notices of the Royal Astronomical Society. 219 (3): 629–655. Bibcode:1986MNRAS.219..629W. doi:10.1093/mnras/219.3.629.
- 1 2 3 4 5 6 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.
- ↑ Watson, C. L.; Henden, A. A.; Price, A. (May 2006). "The International Variable Star Index (VSX)". Society for Astronomical Sciences Annual Symposium. 25: 47. Bibcode:2006SASS...25...47W.
- ↑ Wade, Richard A.; Horne, Keith (January 1988). "The radial velocity curve and peculiar TiO distribution of the red secondary star in Z Chamaeleontis". The Astrophysical Journal. 324: 411. Bibcode:1988ApJ...324..411W. doi:10.1086/165905. eISSN 1538-4357. ISSN 0004-637X.
- ↑ 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. ISSN 1063-7729. S2CID 255195566.
- ↑ Duflot, M.; Figon, P.; Meyssonnier, N. (December 1995). "Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue". Astronomy and Astrophysics Supplement Series. 114: 269. Bibcode:1995A&AS..114..269D. ISSN 0365-0138.
- 1 2 McAllister, M; Littlefair, S P; Parsons, S G; Dhillon, V S; Marsh, T R; Gänsicke, B T; Breedt, E; Copperwheat, C; Green, M J; Knigge, C; Sahman, D I; Dyer, Martin J; Kerry, P; Ashley, R P; Irawati, P (2019-07-11). "The evolutionary status of Cataclysmic Variables: eclipse modelling of 15 systems". Monthly Notices of the Royal Astronomical Society. 486 (4): 5535–5551. arXiv:1904.01888. doi:10.1093/mnras/stz976. ISSN 0035-8711.
- ↑ Marsh, T. R.; Horne, Keith; Shipman, H. L. (April 1987). "A spectrophotometric study of the emission lines in the quiescent dwarf nova Z Chamaeleontis". Monthly Notices of the Royal Astronomical Society. 225 (3): 551–580. Bibcode:1988ApJ...324..411W. doi:10.1093/mnras/225.3.551. eISSN 1365-2966. ISSN 0035-8711.
- 1 2 Dai; Qian, Shengbang; Lajús, Eduardo FernáNdez (26 August 2009). "Evidence of a Brown Dwarf in the Eclipsing Dwarf Nova Z Chamaeleonis". The Astrophysical Journal. 703 (1): 109–113. Bibcode:2009ApJ...703..109D. doi:10.1088/0004-637X/703/1/109.
- ↑ Cannon, Annie J. (1907). "Second catalogue of variable stars". Annals of Harvard College Observatory. 55: 1–94. Bibcode:1907AnHar..55....1C. Retrieved 26 January 2025.
- ↑ Mumford, G. S. (March 1969). "Z Chameleontis" (PDF). Information Bulletin on Variable Stars. 337: 1. Bibcode:1969IBVS..337....1M. Retrieved 26 January 2025.
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