2005A&A...433.1063A


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.19CEST00:25:11

2005A&A...433.1063A - Astronomy and Astrophysics, volume 433, 1063-1077 (2005/4-3)

First detections of the cataclysmic variable AE Aquarii in the near to far infrared with ISO and IRAS: Investigating the various possible thermal and non-thermal contributions.

ABADA-SIMON M., CASARES J., EVANS A., EYRES S., FENDER R., GARRINGTON S., DE JAGER O., KUNO N., MARTINEZ-PAIS I.G., DE MARTINO D., MATSUO H., MOUCHET M., POOLEY G., RAMSAY G., SALAMA A. and SCHULZ B.

Abstract (from CDS):

We have used ISO to observe the Magnetic Cataclysmic Variable AE Aquarii in the previously unexplored range from 4.8µm up to 170µm in the framework of a coordinated multi-wavelength campaign from the radio to optical wavelengths. We have obtained for the first time a spectrum between 4.8 and 7.3µm with ISOCAM and ISOPHOT-P: the major contribution comes from the secondary star spectrum, with some thermal emission from the accretion stream, and possibly some additional cyclotron radiation from the post-shock accretion material close to the magnetised white dwarf. Having reprocessed ISOPHOT-C data, we confirm AE Aqr detection at 90µm and we have re-estimated its upper limit at 170µm. In addition, having re-processed IRAS data, we have detected AE Aqr at 60µm and we have estimated its upper limits at 12, 25, and 100µm. The literature shows that the time-averaged spectrum of AE Aqr increases roughly with frequency from the radio wavelengths up to ∼761µm; our results indicate that it seems to be approximately flat between ∼761 and ∼90µm, at the same level as the 3σ upper limit at 170µm; and it then decreases from ∼90µm to ∼7µm. Thermal emission from dust grains or from a circum-binary disc seems to be very unlikely in AE Aqr, unless such a disc has properties substantially different from those predicted recently. Since various measurements and the usual assumptions on the source size suggest a brightness temperature below 109K at λ≤3.4 mm, we have reconsidered also the possible mechanisms explaining the emission already known from the submillimetre to the radio. The complex average spectrum measured from ∼7µm to the radio must be explained by emission from a plasma composed of more than one ``pure'' non-thermal electron energy distribution (usually assumed to be a power-law): either a very large volume (diameter ≥80 times the binary separation) could be the source of thermal bremsstrahlung which would dominate from ∼10µm to the ∼millimetre, with, inside, a non-thermal source of synchrotron which dominates in radio; or, more probably, an initially small infrared source composed of several distributions (possibly both thermal, and non-thermal, mildly relativistic electrons) radiates gyro-synchrotron and expands moderately: it requires to be re-energised in order to lead to the observed, larger, radio source of highly relativistic electrons (in the form of several non-thermal distributions) which produce synchrotron.

Abstract Copyright:

Journal keyword(s): stars: novae, cataclysmic variables - infrared: stars - radio continuum: stars - stars: flare - radiation mechanisms: thermal - radiation mechanisms: non-thermal

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 HD 8810 * 01 25 05.3072673491 -64 22 10.115869292   7.449 5.900     K5III 30 0
2 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3615 1
3 QSO B1404+286 BLL 14 07 00.3933203928 +28 27 14.695133019   16.13 15.35 10.29   ~ 657 2
4 BD+30 2512 PM* 14 21 57.2162459758 +29 37 46.617158703 11.080 9.840   8.741   K6V 119 0
5 HD 150010 PM* 16 31 28.22748 +72 36 44.4106   7.645 6.304     K2III 22 0
6 V* AM Her AM* 18 16 13.2546541781 +49 52 04.759861155     12.30     M4.5 905 0
7 HD 172323 SB* 18 35 09.3562669174 +63 41 47.341505526       7.8   F9V 46 0
8 * del Dra PM* 19 12 33.3019645 +67 39 41.545581 4.85 4.07 3.07 2.37 1.86 G9III 259 0
9 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 1742 2
10 BD-01 4021 * 20 39 31.5629985452 -00 52 27.095089690   10.17 9.86     A2 2 0
11 V* AE Aqr DQ* 20 40 09.1598509019 -00 52 15.057042857   12.46 10.40   10.191 K3-5IV/V 600 0
12 IRAS F20384-0103 IR 20 41 00.5 -00 52 24           ~ 2 0
13 PMN J2042+0356 Rad 20 42 14.50252437 +03 56 13.9370345           ~ 6 1
14 QSO B2047+03 BLL 20 50 06.2403049172 +04 07 48.887482656   19.8   19.00   ~ 66 1
15 QSO B2059+034 QSO 21 01 38.83416420 +03 41 31.3209577   18.13 17.78 17.68   ~ 144 1
16 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2301 1
17 QSO B2134+0028 QSO 21 36 38.5862648232 +00 41 54.210724774   17.30 17.08 17.02   ~ 515 2

    Equat.    Gal    SGal    Ecl

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2019.10.19-00:25:11

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