Z Chamaeleontis

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Z Chamaeleontis
ZChaLightCurve.png
A light curve for Z Chamaeleontis, adapted from Wood et al. (1986) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Chamaeleon
Right ascension 08h 07m 27.7517s
Declination −76° 32′ 00.6650″
Apparent magnitude  (V)11.5 - 16.2 [2]
Characteristics
Spectral type DA? + M5.5e [3]
Variable type SU UMa + Algol [4]
Astrometry
Radial velocity (Rv)−20 [5]  km/s
Proper motion (μ)RA: −33.650  mas/yr [6]
Dec.: +56.883  mas/yr [6]
Parallax (π)8.2805 ± 0.074  mas [6]
Distance 394 ± 4  ly
(121 ± 1  pc)
Orbit
Primarywhite dwarf
Companionred dwarf
Period (P)1.79  h [7]
Eccentricity (e)0 [7]
Inclination (i)81.8±0.1 [8] °
Semi-amplitude (K1)
(primary)		105 [7] km/s
Details
white dwarf
Mass 1 [8]   M☉
Radius 0.013/0.48  R☉
Luminosity 0.007/0.017  L☉
Temperature 14,700/3100  K
red dwarf
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 [6] 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. [9]

Contents

Z Chamaeleontis was discovered in 1904, during the work required to produce the Astrographic Catalogue. By 1905 a period of variability had been derived. [10] in 1969, George S. Mumford discovered that in addition to being a dwarf nova, the star is an eclipsing variable. [11]

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.

Possible makeup of the Z Chamaeleontis Star system. Diagram of the (possible) Z Chamaeleontis Star system.png
Possible makeup of the Z Chamaeleontis Star system.
The Z Chamaeleontis planetary system [9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(years)		 Eccentricity Inclination Radius
b(unconfirmed)≥20 MJ 9.928≤0.2——

See also

Related Research Articles

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Gamma<sup>3</sup> Octantis Star in the constellation Octans

Gamma3 Octantis, Latinized from γ3 Octantis, is a solitary star located in the southern circumpolar constellation Octans. It is faintly visible to the naked eye as an orange-hued star with an apparent magnitude of 5.28. The object is located relatively close at a distance of 264 light years but is receding with a heliocentric radial velocity of 15 km/s. At its current distance, Gamma3 Octantis' brightness is diminished by two tenths of a magnitude due to interstellar dust and Eggen (1993) lists it as a member of the old disk population. It has an absolute magnitude of +0.83.

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<span class="mw-page-title-main">HD 76236</span> Star in the constellation Chamaeleon

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<span class="mw-page-title-main">DR Chamaeleontis</span> Binary star in the constellation Chamaeleon

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<span class="mw-page-title-main">8 Leonis Minoris</span> Star in the constellation of Leo Minor

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<span class="mw-page-title-main">HD 118285</span> SPB star in the constellation Chamaeleon.

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<span class="mw-page-title-main">HD 59640</span> Suspected eruptive variable in the constellation Volans

HD 59640 is a solitary white hued star located in the southern circumpolar constellation Volans. It has an apparent magnitude of 6.48, placing it near the limit for naked eye visibility. Gaia DR3 parallax measurements place the object at a distance of 262 light years and it is receding with a heliocentric radial velocity of 18.4 km/s. At its current distance, HD 59640's brightness is diminished by three tenths of a magnitude due to interstellar dust.

<span class="mw-page-title-main">HD 75747</span> Star in the constellation Chamaeleon

HD 75747, also known as HR 3524 or RS Chamaeleontis, is a binary star located in the southern circumpolar constellation Chamaeleon. It has an average apparent magnitude of 6.05, making it barely visible to the naked eye. The system is located relatively close at a distance of 322 light years based on Gaia DR3 parallax measurements but is receding with a somewhat constrained heliocentric radial velocity of 16.1 km/s. It has an absolute magnitude of +1.21.

<span class="mw-page-title-main">HD 93486</span> Algol variable in the constellation Chamaeleon

HD 93486, also known as HIP 52381, is a binary star located in the southern circumpolar constellation Chamaeleon near the border with Octans. Its variable star designation is RZ Chamaeleontis. It has an apparent magnitude ranging from 8.2 to 9.1, which is below the limit for naked eye visibility. Gaia DR3 parallax measurements place the system 568 light years away, and it is currently receding with a heliocentric radial velocity of 20 km/s. At its current distance, HD 93486's average brightness is diminished by 0.53 magnitudes due to interstellar dust. The system has a combined absolute magnitude of +1.72.

<span class="mw-page-title-main">T Chamaeleontis</span> T Tauri star; Chamaeleon

T Chamaeleontis, also known as HIP 58285, is a T Tauri star located in the southern circumpolar constellation Chamaeleon. It has an apparent magnitude that ranges from 10.05 to 14.50, which is below the limit for naked eye visibility. Gaia DR3 parallax measurements place the object 335 light years away and it is currently receding with a heliocentric radial velocity of 13.8 km/s. At its current distance, T Cha's average brightness is diminished by 0.31 magnitudes due to extinction from interstellar dust. It has an average absolute magnitude of +6.55.

<span class="mw-page-title-main">V686 Coronae Australis</span> Alpha2 CVn variable; Corona Australis

V686 Coronae Australis is a solitary, bluish-white-hued variable star located in the southern constellation Corona Australis. It has an apparent magnitude that ranges between 5.25 and 5.41, which makes it faintly visible to the naked eye. Gaia DR3 parallax measurements imply a distance of 480 light years and it is slowly receding with a heliocentric radial velocity of 1.3 km/s. At its current distance V686 CrA's average brightness is diminished by 0.35 magnitudes due to extinction from interstellar dust and it has an absolute visual magnitude of −0.24.

<span class="mw-page-title-main">HD 196917</span> Suspected variable star in Microscopium

HD 196917 is a solitary star located in the southern constellation Microscopium. It is faintly visible to the naked eye as a red-hued point of light with an apparent magnitude of 5.74. Gaia DR3 parallax measurements imply a distance of 426 light-years and it is rapidly approaching the Solar System with a heliocentric radial velocity of −97.3 km/s. At its current distance, HD 196917's brightness is diminished by 0.13 magnitudes due to interstellar extinction and it has an absolute magnitude of +0.04.

References

  1. ↑ 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 .
  2. ↑ 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.
  3. ↑ 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.
  4. ↑ 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.
  5. ↑ 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.
  6. 1 2 3 4 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.
  7. 1 2 3 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.
  8. 1 2 Otulakowska-Hypka, Magdalena; Olech, Arkadiusz; Patterson, Joseph (12 May 2016). "Statistical analysis of properties of dwarf novae outbursts". Monthly Notices of the Royal Astronomical Society. 460 (3): 2526–2541. arXiv: 1605.02937 . Bibcode:2016MNRAS.460.2526O. doi: 10.1093/mnras/stw1120 . eISSN   1365-2966. ISSN   0035-8711.
  9. 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 .
  10. ↑ 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.
  11. ↑ 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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