2007A&A...475..575T


C.D.S. - SIMBAD4 rel 1.7 - 2019.09.16CEST23:21:33

2007A&A...475..575T - Astronomy and Astrophysics, volume 475, 575-583 (2007/11-4)

K-band spectroscopy of pre-cataclysmic variables.

TAPPERT C., GAENSICKE B.T., SCHMIDTOBREICK L., MENNICKENT R.E. and NAVARRETE F.P.

Abstract (from CDS):

There exists now substantial evidence for abundance anomalies in a number of cataclysmic variables (CVs), indicating that the photosphere of the secondary star incorporates thermonuclear processed material. However, the spectral energy distribution in CVs is usually dominated by the radiation produced by the accretion process, severely hindering an investigation of the stellar components. On the other hand, depending on how the secondary star has acquired such material, the above mentioned abundance anomalies could also be present in pre-CVs, i.e. detached white/red dwarf binaries that will eventually evolve into CVs, but have not yet started mass transfer, and therefore allow for an unobstructed view on the secondary star at infrared wavelengths. We have taken K-band spectroscopy of a sample of 13 pre-CVs in order to examine them for anomalous chemical abundances. In particular, we study the strength of the 12CO and 13CO absorption bands that have been found diminished and enhanced, respectively, in similar studies of CVs. All our systems show CO abundances that are within the range observed for single stars. The weakest 12CO bands with respect to the spectral type are found in the pre-CV BPM 71214, although on a much smaller scale than observed in CVs. Furthermore there is no evidence for enhanced 13CO. Taking into account that our sample is subject to the present observational bias that favours the discovery of young pre-CVs with secondary stars of late spectral types, we can conclude the following: 1) our study provides observational proof that the CO anomalies discovered in certain CVs are not due to any material acquired during the common envelope phase, and 2) if the CO anomalies in certain CVs are not due to accretion of processed material during nova outburst, then the progenitors of these CVs are of a significantly different type than the currently known sample of pre-CVs.

Abstract Copyright:

Journal keyword(s): stars: binaries: close - stars: late-type - stars: novae, cataclysmic variables - infrared: stars

Simbad objects: 36

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Number of rows : 36

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 G 269-70 CV* 00 59 28.8887547784 -26 31 05.657727154   16.22 15.94     M5.5 36 0
2 V* CC Cet WD* 03 10 54.9905206191 +09 49 25.677202027           DA2+dM 48 0
3 HD 20340 Be* 03 15 45.8642513299 -16 49 43.504779485 7.26 7.83 7.96     B3Ve 51 0
4 V* LL Eri WD* 03 32 43.4695166384 -08 55 39.253882059   14.415 13.60     DA+M2.5V 33 0
5 [RRW93] P83l-57 HS* 03 34 34.3246528495 -64 00 57.112838486 13.04 14.15 14.32     sdB 9 0
6 V* RR Cae WD* 04 21 05.5631969817 -48 39 07.062891386 14.50 14.92 14.40     DA7.8 129 1
7 HD 34686 * 05 19 07.1980081434 -04 57 34.720968146   8.85 8.76     A0V 10 0
8 HD 38087 ** 05 43 00.5750795483 -02 18 45.388281574 7.96 8.40 8.29 8.06 7.89 B3II 145 1
9 HD 45566 * 06 27 36.8564511276 -15 18 22.179824157   7.40 7.49     B3/5V 8 1
10 V* AE Pic bL* 06 31 10.6389999382 -61 52 46.351524024   5.990 6.144     B2V 45 0
11 HD 52018 * 06 58 35.8983203688 -25 24 50.944786089   5.420 5.583     B2V 47 0
12 HD 54995 * 07 10 46.9553893103 -09 20 09.610313992   7.30 7.42     B4/5II/III 13 0
13 RX J1016.4-0520 WD* 10 16 28.6043781785 -05 20 35.222043934     14.1     DAO+Me 101 0
14 BD+20 2465 ** 10 19 36.2808024653 +19 52 12.014037746   10.82 9.52 9.19   M4Vae 1103 0
15 V* V345 Vel Al* 10 22 08.9083669138 -49 17 36.723181163   7.42 7.56     B3V 16 0
16 V* UZ Sex WD* 10 28 34.8776752831 -00 00 29.394108221   13.89   13.9   DA3+dM 73 0
17 WG 17 WD* 10 44 10.2362521693 -69 18 18.076734998   13.05 13.09     DA2+dM 52 0
18 HD 95735 Fl* 11 03 20.19400 +35 58 11.5682 10.030 8.960 7.520 5.99 4.79 M2+V 606 1
19 HD 97991 * 11 16 11.7120502560 -03 28 19.097002665 6.28 7.19 7.41     B2/B3V 127 0
20 HE 1247-1738 WD* 12 50 22.0731640839 -17 54 46.561124536   16.32 16.19 15.7   DA3+dM 17 0
21 HD 116538 bC* 13 25 12.2148493979 -51 50 30.446843244 6.99 7.80 7.88     B2Ib/II 29 0
22 EC 13349-3237 WD* 13 37 50.7137449155 -32 52 21.590040617   16.7 16.34     DA1+dM 13 0
23 V* QS Vir WD* 13 49 52.0031855330 -13 13 37.001934702 14.27 14.98 14.40 14.37   DA3+dM 118 1
24 HE 1432-1625 WD* 14 35 45.6656731277 -16 38 16.938156800   15.14 14.58 15.0   DA3+dM 14 0
25 V* NN Ser No* 15 52 56.1202658103 +12 54 44.432043501   16.0 16.51     DAO1+M4 217 2
26 V* V600 Her Ce* 16 36 58.2041650076 +14 28 30.910552466 5.87 6.845 7.028     B0.5III 151 0
27 HD 164519 PM* 18 03 12.5160964841 -36 32 52.488760390   9.28 8.72     G0V 12 0
28 HD 181132 PM* 19 20 51.6558620513 -38 24 39.848568277   9.74 9.13     G3V 6 0
29 HD 201254 * 21 07 57.4065574609 +14 40 25.257146398 6.220 6.890 7.020     B3V 34 0
30 HD 203617 * 21 23 41.8693361235 -12 03 36.609474336   7.89 8.01     B2/3V 6 0
31 LP 759-25 PM* 22 05 35.7339481228 -11 04 28.961273294   18.4   16.4 13.73 M6Ve 28 0
32 EIS-DEEP HDFS-1 Ks 1 659 * 22 33 15.8015084824 -60 32 24.424971043   15.80 13.95     M2V 4 0
33 V* EZ Aqr BY* 22 38 33.576000 -15 17 59.75700 15.762 14.33 12.38 12.12 8.677 M5V 277 1
34 1RXS J231318.1-493322 PM* 23 13 16.7065414693 -49 33 15.481152277   15.83 14.24 13.85 11.366 M3Ve 15 0
35 HD 219134 Fl* 23 13 16.9747821012 +57 10 06.076520993 7.460 6.560 5.570 4.76 4.23 K3V 496 1
36 Ross 248 BY* 23 41 55.0361186415 +44 10 38.825189497   14.19   11.1   M5.0V 264 0

    Equat.    Gal    SGal    Ecl

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2019.09.16-23:21:33

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