2010A&A...510A..59N


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.08CET08:56:20

2010A&A...510A..59N - Astronomy and Astrophysics, volume 510, A59-59 (2010/2-1)

Hot and cool: two emission-line stars with constrasting behaviours in the same XMM-Newton field.

NAZE Y., RAUW G. and UD-DOULA A.

Abstract (from CDS):

High-energy emissions are good indicators of peculiar behaviours in stars. We have therefore obtained an XMM-Newton observation of HD155806 and 1RXSJ171502.4-333344, and derived their spectral properties for the first time. The X-ray spectrum of HD155806 appears soft, even slightly softer than usual for O-type stars (as shown by a comparison with the O9 star HD155889 in the same XMM-Newton field). It is well-fitted with a two-component thermal model with low temperatures (0.2 and 0.6keV), and it shows no overluminosity (log[LX/LBOL]=-6.75). The high-resolution spectrum, though noisy, reveals a few broad, symmetric X-ray lines (FWHM∼2500km/s). The X-ray emission is compatible with the wind-shock model and therefore appears unaffected by the putative dense equatorial regions at the origin of the Oe classification. 1RXSJ171502.4-333344 is a nearby flaring source of moderate X-ray luminosity (log[LX/LBOL]=-3), with a soft thermal spectrum composed of narrow lines and presenting a larger abundance of elements (e.g. Ne) with a high first ionization potential (FIP) compared to lower-FIP elements. All the evidence indicates a coronal origin for the X-ray emission, in agreement with the dMe classification of this source.

Abstract Copyright:

Journal keyword(s): X-rays: stars - stars: early-type - stars: individual: 1RXSJ171502.4-333344 - stars: individual: HD155806 - stars: emission-line, Be - X-rays: individual: HD155889

Simbad objects: 16

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Number of rows : 16

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * gam Cas Be* 00 56 42.5317 +60 43 00.265 1.18 2.29 2.39 2.32 2.40 B0.5IVpe 1126 2
2 * tet01 Ori C ** 05 35 16.46375 -05 23 22.8486 4.20 5.15 5.13 4.91 4.73 O7Vp 1257 1
3 * zet Ori ** 05 40 45.52666 -01 56 33.2649   1.59 1.79     O9.7Ib+B0III 324 0
4 HD 39680 Be* 05 54 44.7314236108 +13 51 17.068152340 7.05 8.01 7.99     O6V:[n]pevar 111 0
5 * tet Car SB* 10 42 57.4019674 -64 23 40.020796 1.53 2.54 2.76 2.87 3.10 B0Vp 313 0
6 V* RS CVn Al* 13 10 36.9078781154 +35 56 05.587686902 8.57 8.51 7.93 7.7   F6IV+G8IV 679 0
7 HD 119682 Be* 13 46 32.5707617771 -62 55 24.153203600 7.26 7.978 7.901 8.72   B0Ve 50 0
8 Ass Sco OB 4 As* 17 12.6 -33 22           ~ 39 0
9 2MASS J17150219-3333398 Ro* 17 15 02.20 -33 33 39.8     10.933   9.066 M0 16 0
10 USNO-B1.0 0564-00551957 PM* 17 15 02.209 -33 33 39.86       10.3   ~ 1 0
11 1RXS J171518.9-333250 X 17 15 18.905 -33 32 50.50           ~ 1 0
12 HD 155806 Be* 17 15 19.2484405697 -33 32 54.307297319 4.61 5.52 5.53     O7.5V((f))z(e) 202 0
13 HD 155889 ** 17 15 50.7533188725 -33 44 13.256102872 5.68 6.54 6.55 7.60   O9.5IV 77 1
14 Ross 145 PM* 18 41 59.0356870572 +31 49 49.761626262   12.84 13.126 10.845   M2V 58 0
15 Ross 154 Fl* 18 49 49.3638007809 -23 50 10.453568573 13.528 12.235 10.495 9.278 7.703 M3.5Ve 317 0
16 V* AT Mic ** 20 41 51.15925 -32 26 06.8283 12.753 11.909 10.343 9.098 7.383 M4.5Ve+M4.5Ve 320 0

    Equat.    Gal    SGal    Ecl

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2019.12.08-08:56:20

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