2010A&A...517A..72L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.12CEST09:50:59

2010A&A...517A..72L - Astronomy and Astrophysics, volume 517, A72-72 (2010/7-1)

The double-peaked 2008 outburst of the accreting milli-second X-ray pulsar, IGR J00291+5934.

LEWIS F., RUSSELL D.M., JONKER P.G., LINARES M., TUDOSE V., ROCHE P., CLARK J.S., TORRES M.A.P., MAITRA D., BASSA C.G., STEEGHS D., PATRUNO A., MIGLIARI S., WIJNANDS R., NELEMANS G., KEWLEY L.J., STROUD V.E., MODJAZ M., BLOOM J.S., BLAKE C.H. and STARR D.

Abstract (from CDS):

In August 2008, the accreting milli-second X-ray pulsar (AMXP), IGR J00291+5934, underwent an outburst lasting ∼100 days, the first since its discovery in 2004. We present data from the 2008 double-peaked outburst of IGR J00291+5934 from Faulkes Telescope North, the Isaac Newton Telescope, the Keck Telescope, PAIRITEL, the Westerbork Synthesis Radio Telescope and the Swift, XMM-Newton and RXTE X-ray missions. We study the outburst's evolution at various wavelengths, allowing us to probe accretion physics in this AMXP. We study the light curve morphology, presenting the first radio-X-ray spectral energy Distributions (SEDs) for this source and the most detailed UV-IR SEDs for any outbursting AMXP. We show simple models that attempt to identify the emission mechanisms responsible for the SEDs. We analyse short-timescale optical variability, and compare a medium resolution optical spectrum with those from 2004. The outburst morphology is unusual for an AMXP, comprising two peaks, the second containing a ``plateau'' of ∼10 days at maximum brightness within 30 days of the initial activity. This has implications on duty cycles of short-period X-ray transients. The X-ray spectrum can be fitted by a single, hard power-law. We detect optical variability of ∼0.05 mag, on timescales of minutes, but find no periodic modulation. In the optical, the SEDs contain a blue component, indicative of an irradiated disc, and a transient near-infrared (NIR) excess. This excess is consistent with a simple model of an optically thick synchrotron jet (as seen in other outbursting AMXPs), however we discuss other potential origins. The optical spectrum shows a double-peaked Hα profile, a diagnostic of an accretion disc, but we do not clearly see other lines (e.g. He I, II) that were reported in 2004. Optical/IR observations of AMXPs appear to be excellent for studying the evolution of both the outer accretion disc and the inner jet, and may eventually provide us with tight constraints to model disc-jet coupling in accreting neutron stars.

Abstract Copyright:

Journal keyword(s): pulsars: general - X-rays: binaries - stars: neutron - accretion, accretion disks

Simbad objects: 20

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Number of rows : 20

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 V* V709 Cas DQ* 00 28 48.8268573576 +59 17 22.032796584           ~ 113 0
2 V* V1037 Cas LXB 00 29 03.06 +59 34 19.0           ~ 231 1
3 UCAC3 300-10295 * 00 29 05.3094810269 +59 34 20.878189411     15.60     ~ 1 0
4 UCAC3 300-10297 * 00 29 05.3756148112 +59 34 32.151630493     16.02     ~ 1 0
5 PG 0231+051 WD* 02 33 41.3573346299 +05 18 43.652047965 14.562 15.776 16.096 16.267 16.639 DAO.6 136 0
6 V* V1055 Ori LXB 06 17 07.3 +09 08 13   18.80 18.5     ~ 506 1
7 PSR J1023+0038 LXB 10 23 47.6840307966 +00 38 41.006983532     17.31     GV 309 0
8 V* KV UMa HXB 11 18 10.7922353051 +48 02 12.319175505     12.25     K5V-M1V 721 0
9 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3716 1
10 V* BW Cir HXB 13 58 09.700 -64 44 05.80 17.90 18.00 16.9     ~ 192 1
11 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 599 0
12 [VVI2000] X2 XB* 17 48 52.43 -20 21 31.7           ~ 9 1
13 IGR J17511-3057 LXB 17 51 08.55 -30 57 41.7           ~ 86 1
14 [KRL2007b] 291 LXB 17 51 13.49 -30 37 23.4           ~ 228 0
15 V* V4580 Sgr LXB 18 08 27.54 -36 58 44.3   16.81 16.51     ~ 870 0
16 V* V5511 Sgr LXB 18 13 39.03 -33 46 22.3   18.61 18.33 18.05   ~ 175 0
17 2MAXI J1900-248 LXB 19 00 08.65 -24 55 13.7     18.09     ~ 179 0
18 BD+28 4211 HS* 21 51 11.0220905905 +28 51 50.366090892 8.922 10.25 10.58 10.656 10.831 sdO2VIIIHe5 735 0
19 Feige 110 HS* 23 19 58.3995050606 -05 09 56.170282845 10.360 11.45 11.50 11.970 12.145 sdO8VIIIHe5 552 1
20 SDSS J234817.22+005557.2 * 23 48 17.2142309805 +00 55 57.226481052           ~ 2 0

    Equat.    Gal    SGal    Ecl

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2020.07.12-09:50:59

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