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Open Access Articles- Top Results for AE Aquarii

AE Aquarii

AE Aquarii <tr><td colspan="2" style="text-align:center;">
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Artistic illustration of the AE Aquarii system
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Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Aquarius
Right ascension 20h 40m 09.16206s[1]
Declination −00° 52′ 15.0618″[1]
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This page is a soft redirect. Apparent magnitude (V)

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This page is a soft redirect. 11.6[2]

Characteristics
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This page is a soft redirect. Spectral type

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This page is a soft redirect. White dwarf + K4–5 V[3]

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This page is a soft redirect. B−V color index

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This page is a soft redirect. −1.2[2]

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This page is a soft redirect. Variable type

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This page is a soft redirect. DQ Her <tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2">Astrometry</th></tr></th></tr><tr><th colspan="2" style="text-align: center"></tr><tr style="vertical-align:top;"><td>Radial velocity (Rv)</td><td>−53[4] km/s</td></tr><tr style="vertical-align:top;"><td>Proper motion (μ)</td><td> RA: +73.95[1] mas/yr
Dec.: +12.40[1] mas/yr </td></tr><tr style="vertical-align:top;"><td>Parallax (π)</td><td>11.61 ± 2.72[1] mas</td></tr><tr style="vertical-align:top;"><td>Distance</td><td>approx. 280 ly
(approx. 90 pc)</td></tr><tr style="vertical-align:top;"><td>Absolute magnitude (MV)</td><td>~6.6[5]</td></tr><tr><th colspan="2" style="text-align: center"></th></tr> <tr><td style="background-color: #FFFFC0;" colspan="2" align=center>Orbit[6]</td></tr><tr style="vertical-align:baseline;"><td>Period (P)</td><td>9.88 hours</td></tr><tr style="vertical-align:baseline;"><td>Semi-major axis (a)</td><td>2.34 ± 0.02 R</td></tr><tr style="vertical-align:baseline;"><td>Inclination (i)</td><td>70 ± 3°</td></tr> <tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2">Details</th></tr></th></tr><tr><th colspan="2" style="text-align: center">A</th></tr><tr style="vertical-align:baseline;"><td>Mass</td><td>0.63 ± 0.05[6] M</td></tr><tr style="vertical-align:baseline;"><td>Radius</td><td>0.01[7] R</td></tr><tr style="vertical-align:baseline;"><td>Rotation</td><td>33.08 sec[8]</td></tr><tr><th colspan="2" style="text-align: center">B</th></tr><tr style="vertical-align:baseline;"><td>Mass</td><td>0.37 ± 0.04[6] M</td></tr><tr style="vertical-align:baseline;"><td>Radius</td><td>0.79[6] R</td></tr>

<tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2">Other designations</th></tr><tr><td colspan="2">
2E 2037.5-0102, GCRV 71273, 1RXS J204009.4-005216, AN 342.1931, 2E 4404, GSC 05177-00636, SBC7 826, 1AXG J204011-0052, RJHA 119, CSI-01-20376, CDS 1178, HIP 101991, 1E 2037.5-0102, 1ES 2037-01.0, 2MASS J20400915-0052151, AAVSO 2035-01.[2]
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<tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2">Database references</th></tr><tr style="vertical-align: top;"><td>SIMBAD</td><td>data</tr>

AE Aquarii is a cataclysmic variable binary star of the DQ Herculis type. Based upon parallax measurements, the system is located at a distance of about Script error: No such module "convert". from the Earth.[1] Because of its unique properties, this system has been subject to a number of scientific studies.[3]

The AE Aquarii system consisting of an ordinary star in a close orbit around a magnetic white dwarf; the pair orbit each other with a period of 9.88 hours. The white dwarf primary has 63% of the Sun's mass but a radius of only about 1% of the Sun. As of 2009, it has the shortest known spin period of any white dwarf, completing a full revolution every 33.08 seconds. This spin is decreasing at a rate of 1.78 ns per year, which is unusually high.[3] The secondary star has a stellar classification of K4-5 V, making it a main sequence star that is generating energy at its core through the thermonuclear fusion of hydrogen. It has about 37% of the Sun's mass but 79% of the Sun's radius.

This system displays flare activity that has been observed across multiple bands of the electromagnetic spectrum, including X-rays. Mass is being lost from the secondary star, most of which is being flung out of the system by the rapidly spinning magnetic primary. The X-ray luminosity is likely being caused by the accretion of mass onto the white dwarf, which is occurring at an estimated rate of about 7.3 × 1010 kg per second.[3]

See also

References

  1. ^ a b c d e f van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. Bibcode:2007A&A...474..653V. arXiv:0708.1752. doi:10.1051/0004-6361:20078357. 
  2. ^ a b c V* AE Aqr, database entry, SIMBAD. Accessed on line July 22, 2008.
  3. ^ a b c d Mauche, Christopher W. (November 2009), "Chandra High-Energy Transmission Grating Spectrum of AE Aquarii", The Astrophysical Journal 706 (1): 130–141, Bibcode:2009ApJ...706..130M, arXiv:0910.0084, doi:10.1088/0004-637X/706/1/130 
  4. ^ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick, Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, University of Toronto: International Astronomical Union, Bibcode:1967IAUS...30...57E 
  5. ^ From apparent magnitude and parallax.
  6. ^ a b c d Echevarría, J. et al. (July 2008). "High-dispersion absorption-line spectroscopy of AE Aqr". Monthly Notices of the Royal Astronomical Society 387 (4): 1563–1574. Bibcode:2008MNRAS.387.1563E. arXiv:0804.0291. doi:10.1111/j.1365-2966.2008.13248.x. 
  7. ^ Itoh, Kei et al. (2005). "Density diagnostics of the hot plasma in AE Aquarii with XMM-NEWTON" (PDF). Proceedings of 'The X-ray Universe 2005', El Escorial, Madrid, Spain: 1–6. Bibcode:2006ApJ...639..397I. doi:10.1086/499152. 
  8. ^ Patterson, Joseph (December 15, 1979). "Rapid oscillations in cataclysmic variables. III. An oblique rotator in AE Aquarii". Astrophysical Journal 234: 1–992. Bibcode:1979ApJ...234..978P. doi:10.1086/157582. 

External links

Coordinates: Sky map 20h 40m 09.1629s, −00° 52′ 15.071″