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J/A+A/606/A130      List of 1254 X-ray bursts                 (in't Zand+, 2017)

Neutron star cooling and the rp process in thermonuclear X-ray bursts. in't Zand J.J.M., Visser M.E.B., Galloway D.K., Chenevez J., Keek L., Kuulkers E., Sanchez-Fernandez C., Worpel H. <Astron. Astrophys. 606, A130 (2017)> =2017A&A...606A.130I (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, X-ray Keywords: X-rays: binaries - X-rays: bursts - stars: neutron - nuclear reactions, nucleosynthesis, abundances Abstract: When the upper layer of an accreting neutron star experiences a thermonuclear runaway of helium and hydrogen, it exhibits an X-ray burst of a few keV with a cool-down phase of typically 1 minute. When there is a surplus of hydrogen, hydrogen fusion is expected to simmer during that same minute due to the rp process, which consists of rapid proton captures and slow β-decays of proton-rich isotopes. We have analyzed the high-quality light curves of 1254 X-ray bursts, obtained with the Proportional Counter Array on the Rossi X-ray Timing Explorer between 1996 and 2012, to systematically study the cooling and rp process. This is a follow-up of a study on a selection of 37 bursts from systems that lack hydrogen and show only cooling during the bursts.We find that the bolometric light curves are well described by the combination of a power law and a one-sided Gaussian. The power-law decay index is between 1.3 and 2.1 and similar to that for the 37-bursts sample. There are individual bursters with a narrower range. The Gaussian is detected in half of all bursts, with a typical standard deviation of 50s and a fluence ranging up to 60% of the total fluence. The Gaussian appears consistent with being due to the rp process. The Gaussian fluence fraction suggests that the layer where the rp process is active is underabundant in H by a factor of at least five with respect to cosmic abundances. Ninety-four percent of all bursts from ultracompact X-ray binaries lack the Gaussian component, and the remaining 6% are marginal detections. This is consistent with a hydrogen deficiency in these binaries. We find no clear correlation between the power law and Gaussian light-curve components. Description: The list of thermonuclear X-ray bursts that RXTE detected was obtained from the Multi-INstrument Burst ARchive (MINBAR; Galloway et al. 2010, in COSPAR Meeting, Vol. 38, 38th COSPAR Scientific Assembly, 6). In addition to RXTE/PCA data, MINBAR contains the bursts detected with BeppoSAX/WFC (Jager et al., 1997A&AS..125..557J) and the still operational INTEGRAL/JEM-X (Lund et al., 2003A&A...411L.231L). The PCA list in MINBAR consists of 2288 bursts from 60 sources (i.e., this is slightly more than half the currently known burster population). Some sources only exhibited one burst in the PCA (e.g., KS 1741-293), while others had close to 400 (e.g., 4U 1636-536). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 42 60 Sample of 2288 bursts detected with RXTE-PCA from 60 sources (a) and of the selection of 1254 bursts employed in the current study (b) tablec1.dat 123 1254 List of all 1254 bursts included in our analysis
See also: J/A+AS/130/233 : WATCH Solar X-Ray Burst Catalogue (Crosby+ 1998) J/PAZh/32/508 : INTEGRAL hard X-ray Bursts in 2003-2004 (Chelovekov+, 2006) J/ApJS/179/360 : Thermonuclear X-ray bursts observed by RXTE (Galloway+ 2008) J/ApJS/180/192 : BeppoSAX/GRBM gamma-ray Burst Catalog (Frontera+, 2009) J/ApJ/693/1484 : Early optical afterglow catalog (Cenko+, 2009) J/ApJ/701/824 : Afterglows of short & long-duration GRBs (Nysewander+, 2009) J/PAZh/37/651 : INTEGRAL hard X-ray bursts in 2003-2009 (Chelovekov+, 2011) J/ApJ/749/21 : AGNs detected by 60 month Swift/BAT survey (Ajello+, 2012) J/A+A/553/A33 : AGILE Mini-Calorimeter gamma-ray burst catalog (Galli+, 2013 J/A+A/557/A12 : Optical light curves of gamma-ray bursts (Zaninoni+, 2013) J/A+A/581/A125 : UV/Optical/NIR spectroscopy GRB hosts (Kruehler+, 2015) J/ApJ/774/157 : Swift GRBs with X-ray afterglows and z<9.5 (Dainotti+, 2013) J/ApJS/209/20 : Swift GRB catalog with X-ray data (Grupe+, 2013) J/ApJS/224/20 : 10yr of Swift/XRT obs. of GRBs (Yi+, 2016) J/MNRAS/428/729 : GRB Swift X-ray light curves analysis (Margutti+, 2013) J/ApJ/788/30 : Gamma-ray burst flares: X-ray flaring (Swenson+, 2014) J/ApJ/826/45 : GRB X-ray afterglows light curves analysis (Racusin+, 2016) J/ApJS/218/11 : 5 year Fermi/GBM magnetar burst catalog (Collazzi+, 2015) J/MNRAS/449/L6 : Gamma-ray burst Eiso/Lopt (Coward+, 2015) J/MNRAS/464/4545 : Gamma Ray Bursts detected by Swift 2004-2015 (Buchner+ 2017) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 17 A17 --- Name Source name 19- 21 I3 ---- Na Number of bursts detected by RXTE-PCA 23- 25 I3 --- Nb Number of bursts employed in the current study 27- 42 A16 --- Com Comments
Byte-by-byte Description of file: tablec1.dat
Bytes Format Units Label Explanations
1- 17 A17 --- Name Source name 19- 22 I4 --- MINBAR ?=-1 MINBAR identification number (-1 if not yet established) 24- 34 F11.5 d MJD Time of burst start in MJD-UTC 36 A1 --- Flag [0/2] Analysis flag (1) 38 I1 s TimeSCorr ? Manual correction to burst start time (s), if applicable 40- 41 I2 s TimeS ? Start time of data included in model fit, in s since burst start time, if different from 55% criterion 43- 45 I3 s TimeE ? End time of data included in model fit, in s since burst time, if different from 300s 47- 52 F6.3 --- alpha2 Best fit alpha2 value and uncertainty 54- 58 F5.3 --- e_alpha2 rms uncertainty on alpha2 60- 65 F6.2 --- chi2r Reduced chi-squared for fit with power-law model 67- 72 F6.3 --- alpha3 Best fit alpha3 value and uncertainty 74- 79 F6.3 --- e_alpha3 rms uncertainty on alpha3 81- 88 F8.3 --- f ?=-1 Fluence fraction f contained in Gaussian component 90- 98 F9.3 --- e_f ?=-1 rms uncertainty on f 100-107 F8.2 s S Gaussian width 109-117 F9.2 s e_S rms uncertainty on S 119-123 F5.2 --- chi2rG ? Reduced chi-squared for fit with power-law plus Gaussian model
Note (1): Analysis flag as follows: 0 = not included in analysis 1 = power-law model result was included in analysis 2 = power-law plus Gaussian model was included in analysis
Acknowledgements: Jean in't Zand, jeanz(at)sron.nl
(End) Patricia Vannier [CDS] 04-Sep-2017
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