V1315 Aquilae

V1315 Aquilae is a cataclysmic variable star located in the constellation of Aquila. It is a type of cataclysmic variable known as a nova-like variable (NL),[4] specifically a SW Sextantis star.[5][6] Nova-like variables such as these SW Sextantis stars are characterized as having non-magnetic white dwarfs and do not undergo dwarf-nova eruptions.[4] There is some evidence that SW Sextantis stars may contain a magnetic white dwarf.[7][8] 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.[9] It emits the majority of its light in the visible range, which is emitted from the accretion disk.[9] The eclipse depth is 1.8 mag.[10] No description of the donating star has been mentioned.

V1315 Aquilae
Observation data
Epoch 2015.5      Equinox
Constellation Aquila
Right ascension  19h 13m 54.531s
Declination +12° 18′ 03.238″
Apparent magnitude (V) 13.8[1]
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
Astrometry
Radial velocity (Rv)38[2] km/s
Proper motion (μ) RA: -2.381[2] mas/yr
Dec.: -6.360[2] mas/yr
Parallax (π)2.2295 ± 0.0314[2] mas
Distance1,460 ± 20 ly
(449 ± 6 pc)
Orbit
Period (P)201 min[3]
Inclination (i)78.2[1]°
Other designations
V1315 Aql, 2MASS J19135453+1218033, CSV 8130
Database references
SIMBADdata

Nova shell

V1315 Aquilae has a roughly spherical shell of material around it with a maximum mass of 1×10−5 solar masses, which is too small to be related to a planetary nebula or supernova remnant. It is predicted that this shell is the remnant of a nova eruption. This nova eruption is estimated to be roughly 500 to 1200 years old. V1315 Aquilae is the first nova-like star to have been discovered with a nova shell.[4]

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References
  1. 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.
  2. 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.
  3. 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.
  4. 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.
  5. 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. Cite journal requires |journal= (help)
  6. Hoard, D. W. "The Big List of SW-Sextantis Stars".
  7. 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. Cite journal requires |journal= (help)
  8. Hoard, D. H. "The Magnetic Scenario for the SW-Sextantis Stars".
  9. 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.
  10. 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.
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