V1315 Aquilae
 A light curve for V1315 Aquilae, from data taken on 31 August 2004. Adapted from Papadaki et al. (2009)[1] | |
| Observation data Epoch 2015.5 Equinox | |
|---|---|
| Constellation | Aquila |
| Right ascension | 19h 13m 54.531s |
| Declination | +12° 18′ 03.238″ |
| Apparent magnitude (V) | 13.8[2] |
| Characteristics | |
| Evolutionary stage | Nova-like Star |
| B−V color index | 0.48 |
| J−H color index | 0.46 |
| J−K color index | 0.63 |
| Variable type | Eclipsing[citation needed] |
| Astrometry | |
| Radial velocity (Rv) | 38[3] km/s |
| Proper motion (μ) | RA: -2.381[3] mas/yr Dec.: -6.360[3] mas/yr |
| Parallax (π) | 2.2295 ± 0.0314 mas[3] |
| Distance | 1,460 ± 20 ly (449 ± 6 pc) |
| Orbit | |
| Period (P) | 201 min[4] |
| Inclination (i) | 78.2[2]° |
| Other designations | |
V1315 Aql, 2MASS J19135453+1218033, CSV 8130 | |
| Database references | |
| SIMBAD | data |
V1315 Aquilae is a cataclysmic variable star in the north of the equatorial constellation of Aquila. It is in the sub-set of nova-like (NL) variables,[5] specifically a SW Sextantis star (a type of white dwarf-donor star pair).[6][7] These were characterized as having non-magnetic white dwarfs – thus that do not undergo dwarf-nova bright luminations ("eruptions").[5] There is countering evidence for some magnetism.[8][9] Being a SW Sextantis star, V1315 Aquilae has a high rate of mass transfer, so it is in steady-state accretion and in a constant state of outburst.[10] It emits most of its light in the visible range, and this comes from the accretion disk.[10] The eclipse depth is 1.8 mag.[11] No description of the donor star is made.
L. P. Metik discovered the star in 1961. Rather unusually, the discovery paper does not give the celestial coordinates of the object, but instead presents a map showing where the star is located in the sky relative to nearby stars.[12] The star was given its variable star designation, V1315 Aquilae, in 1977.[13]
Nova shell
[edit]V1315 Aquilae has a roughly spherical shell of material around it with a maximal 1×10−5 solar masses (1⁄10000 M☉), which is too small to be any starburst nebula or more advanced supernova remnant. It is consistent with models of a remnant of a nova-scale eruption roughly 500 to 1200 years old (that is, plus the time for the light from this system to travel to the Earth). V1315 Aquilae is the first nova-like system to have been discovered with a nova shell.[5]
References
[edit]- ^ Papadaki, C.; Boffin, H. M. J.; Stanishev, V.; Boumis, P.; Akras, S.; Sterken, C. (May 2009). "Photometric study of selected cataclysmic variables II. Time-series photometry of nine systems". The Journal of Astronomical Data. 15: 1. arXiv:0806.1358. Bibcode:2009JAD....15....1P. Retrieved 20 October 2021.
- ^ a b Szkody, P. (1987-02-01). "A photometric and spectroscopic comparison of the cataclysmic variables on the 2 sides of the period gap and at a specific orbital period". Astrophysics and Space Science. 130 (1–2): 69–73. Bibcode:1987Ap&SS.130...69S. doi:10.1007/BF00654973. ISSN 0004-640X. S2CID 123118847.
- ^ a b c d Bailer-Jones, C. a. L.; Babusiaux, C.; de Bruijne, J. H. J.; Prusti, T.; Vallenari, A.; Brown, A. G. A.; Collaboration, Gaia (2018-04-25). "Gaia Data Release 2. Summary of the contents and survey properties". Astronomy and Astrophysics. 616: A1. arXiv:1804.09365v2. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. S2CID 49211658.
- ^ Szkody, Paula; Piche, Francois (1990-09-01). "The phase 0.5 absorption in V1315 Aquilae, SW Sextantis, and DW Ursae Majoris". The Astrophysical Journal. 361: 235–243. Bibcode:1990ApJ...361..235S. doi:10.1086/169188. ISSN 0004-637X.
- ^ a b c Hallinan, G.; Littlefair, S. P.; Dhillon, V. S.; Sahman, D. I. (2018-04-16). "Discovery of an old nova shell surrounding the cataclysmic variable V1315 Aql". Monthly Notices of the Royal Astronomical Society. 477 (4): 4483–4490. arXiv:1804.05596. Bibcode:2018MNRAS.477.4483S. doi:10.1093/mnras/sty950. S2CID 119462899.
- ^ Rutten, R. G. M.; Dhillon, V. S. (1995-06-21). "Spectropolarimetry of the nova-like variable V1315 Aql". arXiv:astro-ph/9506111. doi:10.1093/mnras/277.3.777. S2CID 15959562.
{{cite journal}}: Cite journal requires|journal=(help) - ^ Hoard, D. W. "The Big List of SW-Sextantis Stars". Archived from the original on 2019-04-22. Retrieved 2019-04-22.
- ^ Steeghs, D.; Hakala, P.; Martinez-Pais, I. G.; Casares, J.; Rodriguez-Gil, P. (2000-11-15). "Evidence of magnetic accretion in an SW Sex star: discovery of variable circular polarization in LS Pegasi". arXiv:astro-ph/0011296. doi:10.1086/318922. S2CID 17745748.
{{cite journal}}: Cite journal requires|journal=(help) - ^ Hoard, D. H. "The Magnetic Scenario for the SW-Sextantis Stars". Archived from the original on 2019-04-22. Retrieved 2019-04-22.
- ^ a b Rutten, R. G. M.; van Paradijs, J.; Tinbergen, J. (1992-07-01). "Reconstruction of the accretion disk in six cataclysmic variable stars". Astronomy and Astrophysics. 260: 213–226. Bibcode:1992A&A...260..213R. ISSN 0004-6361.
- ^ Szkody, Paula (1987-10-01). "Time-resolved IUE studies of cataclysmic variables. I - Eclipsing systems IP Peg, PG 1030+590, and V1315 AQL". The Astronomical Journal. 94: 1055–1061. Bibcode:1987AJ.....94.1055S. doi:10.1086/114540. ISSN 0004-6256.
- ^ Metik, L. P. (1961). "Seven New Variable Stars in the Region of Aquilae and SA 87". Peremennye Zvezdy. 13: 364. Bibcode:1961PZ.....13..364M. Retrieved 21 November 2024.
- ^ Kukarkin, B. V.; Kholopov, P. N.; Fedorovich, V. P.; Kireyeva, N. N.; Kukarkina, N. P.; Medvedeva, G. I.; Perova, N. B. (March 1977). "62nd Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 1248: 1–25. Bibcode:1977IBVS.1248....1K. Retrieved 21 November 2024.
