Z Andromedae
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Andromeda |
Right ascension | 23h 33m 39.9551s[1] |
Declination | +48° 49′ 05.975″[1] |
Apparent magnitude (V) | 7.7 - 11.3[2] |
Characteristics | |
Spectral type | M2III + B1eq[3] |
U−B color index | −0.49[4] |
B−V color index | +1.35[4] |
Variable type | Z And[2] |
Astrometry | |
Radial velocity (Rv) | -0.59[5] km/s |
Proper motion (μ) | RA: -1.577 ± 0.111[1] mas/yr Dec.: -3.031 ± 0.134 [1] mas/yr |
Parallax (π) | 0.62 ± 0.40 mas[1] |
Distance | approx. 5,000 ly (approx. 2,000 pc) |
Orbit | |
Period (P) | 759.0±1.9[6] days |
Eccentricity (e) | 0.0[6] |
Inclination (i) | 47±12[7]° |
Semi-amplitude (K1) (primary) | 6.73±0.22[6] km/s |
Details | |
Red giant | |
Mass | 2[6] M☉ |
Radius | 85[3] R☉ |
Luminosity | 880[8] L☉ |
Temperature | 3,400[3] K |
White dwarf | |
Mass | 0.75[6] M☉ |
Radius | 0.17 - 0.36[9] R☉ |
Luminosity | 1,500 - 9,800[9] L☉ |
Temperature | 90,000 - 150,000[9] K |
Rotation | 1682.6 ± 0.6 s[10] |
Other designations | |
Database references | |
SIMBAD | data |
Data sources: | |
Hipparcos Catalogue, CCDM (2002), Bright Star Catalogue (5th rev. ed.) |
Z Andromedae is a binary star system consisting of a red giant and a white dwarf. It is the prototype of a type of cataclysmic variable star known as symbiotic variable stars or simply Z Andromedae variables. The brightness of those stars varies over time, showing a quiescent, more stable phase and an active one with a more pronounced variability and brightening.[11]
Binary system
Z Andromedae is a binary star. The two components have a circular orbit that takes 759 days to complete.[6] The red giant is around twice the mass of the sun and 880 times its luminosity, but its effective temperature is only 2,800 K. The white dwarf is around a thousand times the luminosity of the sun during the quiescent phase, but up to 10 times more luminous during the active phases. Its temperature is as high as 150,000 K when quiescent, but drops below 100,000 K when active.[9] It also spins around its rotation axis every 1682 seconds and displays a strong magnetic field.[10]
The evolved red giant star is losing mass, since radiation pressure overcomes the low gravity on the surface. The outflow of matter is captured by the gravitational field of the white dwarf and falls on its surface in the end. At least during the active phase an accretion disk forms around the white dwarf.[12]
Variability
During the quiescent phase, most the white dwarf luminosity comes from stable hydrogen burning on its surface, and photons emitted this way ionize the wind of the red giant which causes nebular emission. The giant star, however, follows a quasi-periodic activity cycle (similar to the solar cycle) roughly every 7550 days; when the activity of the star is enhanced, the stellar wind becomes stronger, and in response the white dwarf increases in size and cools, triggering the active phase.[7]
In the quiescent phase, the brightness of Z Andromedae is modulated by the orbital period of the system, and can reach a magnitude of mv = 11.3 at his minimum. During the active phase Z Andromedae makes luminosity outbursts and can increase his brightness up to a magnitude of mv = 7.7. Eclipses from the red giant are still visible in this phase. During this phase, a shorter periodicity of 685 days is observed; this could be a beat period between the unknown rotation period of the giant star and the orbital period, which arise from the non-spherical outflow of matter from the atmosphere of the giant star.[8][2][7]
Currently, Z Andromedae is undergoing a long-standing active phase that began in September 2000, and has not yet returned in the quiescent phase due to several optical brightenings. During the outbursts, irregular brightness variations (up to 0.065 magnitudes) were observed at timescales shorter than a day, interpeted as warping in the accretion disk. If models for this source are correct, it should enter a quiescent phase again in 2020.[12]
Spectrum
Optical
The spectrum of Z Andromedae has been recognised as extremely peculiar since the early 20th century. Early spectra during a bright period, showing only emission lines against a red continuum, were interpreted as a star embedded in dense nebulosity.[13] As the star's brightness faded, the spectrum lost the high excitation "nebular" lines and developed absorption lines with P Cygni profiles. These spectra were readily identified as being due to a hot nova-like star with a cool companion.[14] Emission lines identified included low ionization states of hydrogen and helium with high ionization states of oxygen and iron.[9]
The MK spectral classification is typically of a cool giant, for example M4.5.[3] The exact spectral type has been shown to vary, for example between M5 in 1987 and M3.5 in 1989.[15] Infrared observations gave a combination spectral type of M2III + B1eq. Here the luminosity class of III is for a normal giant star, and the peculiarity codes eq indicate emission lines with P Cygni profiles.[3]
Ultraviolet
Z Andromedae shows also a strong ultraviolet emission, which follows the optical behaviour; absorption lines identified during the quiescent phase becomes emission lines during outbursts. Elements identified in this region of the spectrum are carbon, nitrogen, phosphorus and silicon in their ionized states.[9]
Radio
The radio flux from Z Andromedae at the beginning of outbursts is lower than the usual quiescent level, and has a maximum after the optical one. After the outbursts, radio jets can be seen flowing out of this system, in a direction perpendicular to the orbital plane.[9]
X-Ray
Z Andromedae is much fainter in X-ray, and has not been detected when in the quiescent phase. During outbursts, X-ray emission comes from shock-heated plasma, where the kinetic energy of the outflowing material is converted in X-ray radiation. This emission "mimicks" a blackbody radiation with a temperature different from the one of the white dwarf, but its real nature can be identified because it shows absorption edges (which shows also the presence of neon) and an excess at high frequencies.[9]
Bipolar jets
Following the 2006 outburst, the hydrogen Balmer emission lines included faint wings at a velocity of ±1,150 km/s. Since extended radio outflows had previously been seen during the long 2000-2002 outbursts, collimated jets along the axis of the system were the most likely explanation for this phenomenon. It is thought that the jets are only present during bright outbursts.[16] The jets were observed again during subsequent outbursts; their velocity is highly variable at the beginning but settles on a constant velocity after roughly 1 month. A single jet can also occur. The jets could be formed by material that cannot accrete on the white dwarf that reaches the Eddington limit.[12]
References
- ^ a b c d e Gaia Collaboration; Brown, A. G. A; Vallenari, A; Prusti, T; De Bruijne, J. H. J; Mignard, F; Drimmel, R; Babusiaux, C; Bailer-Jones, C. A. L; Bastian, U; Biermann, M; Evans, D. W; Eyer, L; Jansen, F; Jordi, C; Katz, D; Klioner, S. A; Lammers, U; Lindegren, L; Luri, X; O'Mullane, W; Panem, C; Pourbaix, D; Randich, S; Sartoretti, P; Siddiqui, H. I; Soubiran, C; Valette, V; Van Leeuwen, F; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy & Astrophysics. 595: A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512.
- ^ a b c 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.
- ^ a b Martel, M. T; Gravina, R (1985). "UBV Observations of Symbiotic Stars in July and October 1982". Information Bulletin on Variable Stars. 2750: 1. Bibcode:1985IBVS.2750....1M.
- ^ Pourbaix, D; Tokovinin, A. A; Batten, A. H; Fekel, F. C; Hartkopf, W. I; Levato, H; Morrell, N. I; Torres, G; Udry, S (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213.
- ^ a b c d e f Fekel, Francis C; Hinkle, Kenneth H; Joyce, Richard R; Skrutskie, Michael F (2000). "Infrared Spectroscopy of Symbiotic Stars. II. Orbits for Five S-Type Systems with Two-Year Periods". The Astronomical Journal. 120 (6): 3255. Bibcode:2000AJ....120.3255F. doi:10.1086/316872.
- ^ a b c Leibowitz, Elia M; Formiggini, Liliana (2008). "Activity cycle of the giant star of Z Andromedae and its spin period". Mon. Not. R. Astron. Soc. 385: 445. arXiv:0712.2120. Bibcode:2008MNRAS.385..445L. doi:10.1111/j.1365-2966.2008.12847.x.
{{cite journal}}
: CS1 maint: unflagged free DOI (link) - ^ a b Skopal, A (2003). "Discovery of the eclipse in the symbiotic binary Z Andromedae". The Astrophysical Journal. 401 (3): L17. arXiv:astro-ph/0304046. Bibcode:2003A&A...401L..17S. doi:10.1051/0004-6361:20030332.
- ^ a b c d e f g h Sokoloski, J. L; Kenyon, S. J; Espey, B. R; Keyes, Charles D; McCandliss, S. R; Kong, A. K. H; Aufdenberg, J. P; Filippenko, A. V; Li, W; Brocksopp, C; Kaiser, Christian R; Charles, P. A; Rupen, M. P; Stone, R. P. S (2006). "A Combination Nova Outburst in Z Andromedae: Nuclear Shell Burning Triggered by a Disk Instability". The Astrophysical Journal. 636 (2): 1002. arXiv:astro-ph/0509638. Bibcode:2006ApJ...636.1002S. doi:10.1086/498206.
- ^ a b Sokoloski, J. L; Bildsten, Lars (1999). "Discovery of a Magnetic White Dwarf in the Symbiotic Binary Z Andromedae". The Astrophysical Journal. 517 (2): 919. arXiv:astro-ph/9812294. Bibcode:1999ApJ...517..919S. doi:10.1086/307234.
- ^ "Z Andromedae star". Retrieved 2018-01-16.
- ^ a b c Skopal, A.; Tarasova, T. N.; Wolf, M.; Dubovský, P. A.; Kudzej, I. (2018). "Repeated Transient Jets from a Warped Disk in the Symbiotic Prototype Z And: A Link to the Long-lasting Active Phase". The Astrophysical Journal. 858. Bibcode:2018ApJ...858..120S. doi:10.3847/1538-4357/aabc11.
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: CS1 maint: unflagged free DOI (link) - ^ Plaskett, J. S (1928). "The composite stellar and nebular spectrum of Z Andromedae". Publications of the Dominion Astrophysical Observatory Victoria. 4: 119. Bibcode:1928PDAO....4..119P.
- ^ Swings, P; Struve, O (1941). "The Evolution of a Peculiar Stellar Spectrum: Z Andromedae". Astrophysical Journal. 93: 356. Bibcode:1941ApJ....93..356S. doi:10.1086/144272.
- ^ Mürset, U; Schmid, H. M (1999). "Spectral classification of the cool giants in symbiotic systems". Astronomy and Astrophysics Supplement. 137 (3): 473. Bibcode:1999A&AS..137..473M. doi:10.1051/aas:1999105.
- ^ Burmeister, M; Leedjärv, L (2006). "Evidence for bipolar jets from the optical spectra of the prototypical symbiotic star Z Andromedae". The Astrophysical Journal. 461: L5. arXiv:astro-ph/0611475. Bibcode:2007A&A...461L...5B. doi:10.1051/0004-6361:20066630.
Further reading
- Tomov, N. A; Tomova, M. T; Taranova, O. G (2004). "Broad-band multicolour observations of the symbiotic binary Z And during quiescence and its activity at the end of 2002". The Astrophysical Journal. 428 (3): 985. Bibcode:2004A&A...428..985T. doi:10.1051/0004-6361:20041065.
- Taranova, O. G; Tomov, N. A; Tomova, M. T; Shenavrin, V. I (2004). "The symbiotic system Z Andromedae during the flare of 2000–2002". Astronomy Reports. 48 (9): 742. Bibcode:2004ARep...48..742T. doi:10.1134/1.1800174.
- Tomov, N. A; Taranova, O. G; Tomova, M. T (2003). "Mass ejection by the symbiotic binary Z And during its 2000–2002 outburst". The Astrophysical Journal. 401 (2): 669. Bibcode:2003A&A...401..669T. doi:10.1051/0004-6361:20030140.
- Sokoloski, J. L; Brocksopp, C; Kaiser, C; Seymour, N (2002). "A Radio "Jet" in the Prototypical Symbiotic Star Z Andromedae?". American Astron. Soc. Meeting. 201: 17.12. Bibcode:2002AAS...201.1712S.
- Bisikalo, D. V; Boyarchuk, A. A; Kilpio, E. Yu; Kuznetsov, O. A (2002). "Structure of gas flows in Z and in quiescence and during outbursts". Astronomy Reports. 46 (12): 1022. Bibcode:2002ARep...46.1022B. doi:10.1134/1.1529260.
- Birriel, Jennifer J; Espey, Brian R; Schulte-Ladbeck, Regina E (1998). "Near-simultaneous Observations of Direct and Raman-scattered Linesin the Symbiotic Star Z Andromedae". The Astrophysical Journal. 507: L75. Bibcode:1998ApJ...507L..75B. doi:10.1086/311673.
- Schmid, H. M; Schild, H (1997). "The polarimetric orbit of Z Andromedae". Astronomy & Astrophysics. 327: 219. Bibcode:1997A&A...327..219S.
- Skopal, A; Vittone, A. A; Errico, L; Otsuka, M; Tamura, S; Wolf, M; Elkin, V. G (2006). "Structure of the hot object in the symbiotic prototype Z Andromedae during its 2000–03 active phase". The Astrophysical Journal. 453: 279. arXiv:astro-ph/0603718. Bibcode:2006A&A...453..279S. doi:10.1051/0004-6361:20052917.
- Skopal, A; Pribulla, T (2006). "The first detection of the bipolar jets from the symbiotic prototype Z and". The Astronomer's Telegram. 882. Bibcode:2006ATel..882....1S.
- Tomov, N. A; Tomova, M. T; Bisikalo, D. V (2007). "Bipolar ejection by the symbiotic binary system Z and during its 2006 outburst". Mon. Not. R. Astron. Soc. 376: L16. arXiv:astro-ph/0612502. Bibcode:2007MNRAS.376L..16T. doi:10.1111/j.1745-3933.2007.00277.x.
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: CS1 maint: unflagged free DOI (link)