J/ApJ/819/46 Models of thermonuclear X-ray bursters (Lampe+, 2016)
The influence of accretion rate and metallicity on thermonuclear bursts:
predictions from Kepler models.
Lampe N., Heger A., Galloway D.K.
<Astrophys. J., 819, 46 (2016)>
=2016ApJ...819...46L 2016ApJ...819...46L (SIMBAD/NED BibCode)
ADC_Keywords: Models ; X-ray sources ; Accretion
Keywords: stars: neutron; X-rays: bursts
Abstract:
Using the KEPLER 1D hydrodynamics code (Woosley et al.
2004ApJS..151...75W 2004ApJS..151...75W), 464 models of thermonuclear X-ray bursters were
performed across a range of accretion rates and compositions. We
present the library of simulated burst profiles from this sample, and
examine variations in the simulated light curve for different model
conditions. We find that the recurrence time varies as a power law
against accretion rate, and measure its slope while mixed H/He burning
is occurring for a range of metallicities, finding the power law
gradient to vary from η=1.1 to 1.24. We identify the accretion
rates at which mixed H/He burning stops and a transition occurs to
different burning regimes. We explore how varying the accretion rate
and metallicity affects burst morphology in both the rise and tail.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 174 461 Mean model parameters
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See also:
J/A+A/545/A120 : X-ray bursting neutron star atmos. models. II (Suleimanov+,
2012)
J/ApJ/747/77 : Thermonuclear X-ray bursts. II. Eddington limit (Guver+, 2012)
J/ApJS/179/360 : Thermonuclear X-ray bursts observed by RXTE (Galloway+, 2008)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- model Model identifier
6- 7 I2 --- N [0/66] Number of simulated bursts
9- 12 F4.1 % Z [0/20] Metallicity mass fraction
14- 18 F5.2 % H [0/76] Hydrogen mass fraction
20- 25 F6.3 --- Lacc [0.002/50] Accretion luminosity (1)
27- 32 F6.1 s bstLgth [10/2063]? Time length of burst
34- 38 F5.1 s e_bstLgth [0.3/280]? Error in bstLgth
40- 44 F5.2 10+30W pkLum [3.7/69.1]? Burst peak luminosity
46- 50 F5.2 10+30W e_pkLum [0.06/12]? Error in pkLum
52- 56 F5.2 10+28W psLum [0.07/59.3]? Burst persistent luminosity
58- 62 F5.2 10+28W e_psLum [0.01/22]? Error in psLum
64- 69 F6.2 10+32W Fluence [0.4/116.5]? Burst fluence
71- 74 F4.2 10+32W e_Fluence [0.01/7]? Error in Fluence
76- 80 F5.1 s tau [2.4/220]? Equivalent burst duration
82- 85 F4.1 s e_tau [0/36]? Error in tau
87- 92 F6.2 h tDel [0.01/288]? Recurrence time
94- 98 F5.2 h e_tDel [0/15]? Error in tDel
100-105 F6.2 % conv [-19.2/61.7]? Convexity
107-111 F5.2 % e_conv [0/25.2]? Error in conv
113-117 F5.3 s r1090 [0.06/8]? The 10%-90% rise time
119-123 F5.3 s e_r1090 [0.005/2.2]? Error in r1090
125-129 F5.3 s r2590 [0.05/6.6]? The 25%-90% rise time
131-135 F5.3 s e_r2590 [0.001/2]? Error in r2590
137-141 F5.2 --- alpha1 [0.07/10.7]? Power law decay index
143-146 F4.2 --- e_alpha1 [0.01/6.2]? Error in alpha1
148-152 F5.2 s tau1 [1/99]? Exponential decay timescale
154-158 F5.2 s e_tau1 [0.03/29.2]? Error in tau1
160-164 F5.1 --- alpha [36.5/513]? Fluence ratio
166-170 F5.1 --- e_alpha [0.1/591]? Error in alpha
172-174 I3 --- Flag [0/20] Analysis quality flag (2)
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Note (1): As a fraction of eddington luminosity Accretion rate equal to
Lacc*1.75e-8Msun/yr
Luminosity = Lacc*2.05e+38erg/s
Luminosity is relative to Eddington luminosity for a hydrogen
fraction of X=0.7
Note (2): Summed, base 2 values.
0 = No analysis issues.
1 = Burst at end of file (last burst not analysed).
2 = Shocks occur that cause luminosity to exceed L>1e39erg/s.
4 = Bursts have been cut at a local minimum rather than by
luminosity.
8 = Bursts in this train are twin peaked, convexity should not
really be considered for these models.
16 = Rapid bursts with recurrence time less than 100s, This may
indicate some bursts are missed, or the observations include
multiple bursts Often these missed bursts are low intensity
bursts.
32 = Burst not conducive to analysis.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 17-May-2016