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 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 1997A&AS..125..557J) and the still operational
INTEGRAL/JEM-X (Lund et al., 2003A&A...411L.231L 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: tablec1.dat
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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- 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
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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
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Acknowledgements:
Jean in't Zand, jeanz(at)sron.nl
(End) Patricia Vannier [CDS] 04-Sep-2017