J/A+A/527/A139 X-ray bursting neutron star atmosphere models (Suleimanov+, 2011)
X-ray bursting neutron star atmosphere models: spectra and color corrections.
Suleimanov V., Poutanen J., Werner K.
<Astron. Astrophys. 527, A139 (2011)>
=2011A&A...527A.139S 2011A&A...527A.139S
ADC_Keywords: Models, atmosphere ; Binaries, X-ray
Keywords: radiative transfer - scattering - methods: numerical -
stars: neutron - stars: atmospheres - X-rays: stars
Abstract:
X-ray bursting neutron stars in low mass X-ray binaries constitute
an appropriate source class to constrain masses and radii of neutron
stars, but a sufficiently extended set of corresponding model
atmospheres is necessary for these investigations. Methods. We
computed such a set of model atmospheres and emergent spectra in
a plane-parallel, hydrostatic, and LTE approximation with Compton
scattering taken into account.
Description:
There are 18 sets of models for six chemical composition (pure
hydrogen X=1, pure helium Y=1, and four sets of a solar mix of
hydrogen and helium X=0.7374 with various heavy element abundances
Z=1, 0.3, 0.1, and 0.01Z☉; Z☉=0.0134) and three gravities
with logg=14.0, 14.3, and 14.6 (g in units cm/s2). Each of these
18 sets is also characterized by the Eddington temperature at the
surface, neutron star radius (computed for the assumed mass 1.4M☉),
and the redshift, as detailed in set.dat file.
tablea1.dat, for each of the 18 sets there are 20 lines of data
(for 20 values of l and corresponding effective temperatures) containing
color corrections computed by five different procedures described in the
paper. The product of dilution factor and fc4 are also given for the
procedures 1-3.
They are computed from the models presented in tablea2.dat.
For each set, 20 models are computed for relative luminosities (in
units of Eddnington) l=L/L_Edd = 0.001, 0.003, 0.01, 0.03, 0.05, 0.07,
0.1, 0.15, 0.2, 0.3, 0.4, 0.5, 0.6, 0.7, 0.75, 0.8, 0.85, 0.9, 0.95,
0.98.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
set.dat 46 18 Set parameters
tablea1.dat 62 360 Color and dilution factors
tablea2.dat 278 4968 *Atmosphere model spectra
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Note on tablea2.dat: 360 models of neutron star atmospheres.
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Byte-by-byte Description of file: set.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Set [1/18] Set number
4- 9 F6.4 --- X X (H) abundance (0, 0.7374, 1)
11- 16 F6.4 --- Y Y (He) abundance
(0, 0.2492, 0.2586, 0.2613, 0.2625, 1)
18- 24 E7.3 --- Z Z abundance
(0, 1.34E-2, 4.02E-3, 1.34E-3, 1.34E-4)
26- 29 F4.1 [cm/s2] logg Surface gravity (14.0, 14.3, 14.6)
31- 35 F5.3 keV Tedd Eddington temperature (9 values)
37- 41 F5.2 km R Neutron star radius (8.16, 10.88, 14.80)
43- 46 F4.2 --- z Redshift (0.18, 0.27, 0.42)
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Set [1/18] Set number
4- 8 F5.3 --- l Relative luminosity L/Ledd (1)
10- 14 F5.3 keV Teff Effective temperature
16- 20 F5.3 --- fc1 Color correction factor fc,1 (2)
22- 26 F5.3 --- fc2 Color correction factor fc,2 (2)
28- 32 F5.3 --- fc3 Color correction factor fc,3 (2)
34- 38 F5.3 --- fc4 Color correction factor fc,4 (2)
40- 44 F5.3 --- fc5 Color correction factor fc,5 (2)
46- 50 F5.3 --- w*fc1+4 Product of dilution factor and (fc1)4
52- 56 F5.3 --- w*fc2+4 Product of dilution factor and (fc2)4
58- 62 F5.3 --- w*fc3+4 Product of dilution factor and (fc3)4
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Note (1): 20 values from 0.001 to 0.980.
Note (2): where fc=sqrt[R(1+z)/Rbb], where Rbb is the blackbody radius
and R the neutron star radius.
fc1 to fc5 corresponds to the different procedures to determine fc.
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Set Set number
9- 18 E10.5 keV E Photon energy
22- 31 E10.5 mW/m2/keV F(001) Flux FE for l=0.001 (1)
35- 44 E10.5 mW/m2/keV F(003) Flux FE for l=0.003 (1)
48- 57 E10.5 mW/m2/keV F(010) Flux FE for l=0.01 (1)
61- 70 E10.5 mW/m2/keV F(030) Flux FE for l=0.03 (1)
74- 83 E10.5 mW/m2/keV F(050) Flux FE for l=0.05 (1)
87- 96 E10.5 mW/m2/keV F(070) Flux FE for l=0.07 (1)
100-109 E10.5 mW/m2/keV F(100) Flux FE for l=0.1 (1)
113-122 E10.5 mW/m2/keV F(150) Flux FE for l=0.15 (1)
126-135 E10.5 mW/m2/keV F(200) Flux FE for l=0.2 (1)
139-148 E10.5 mW/m2/keV F(300) Flux FE for l=0.3 (1)
152-161 E10.5 mW/m2/keV F(400) Flux FE for l=0.4 (1)
165-174 E10.5 mW/m2/keV F(500) Flux FE for l=0.5 (1)
178-187 E10.5 mW/m2/keV F(600) Flux FE for l=0.6 (1)
191-200 E10.5 mW/m2/keV F(700) Flux FE for l=0.7 (1)
204-213 E10.5 mW/m2/keV F(750) Flux FE for l=0.75 (1)
217-226 E10.5 mW/m2/keV F(800) Flux FE for l=0.8 (1)
230-239 E10.5 mW/m2/keV F(850) Flux FE for l=0.85 (1)
243-252 E10.5 mW/m2/keV F(900) Flux FE for l=0.9 (1)
256-265 E10.5 mW/m2/keV F(950) Flux FE for l=0.95 (1)
269-278 E10.5 mW/m2/keV F(980) Flux FE for l=0.98 (1)
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Note (1): Values of the flux FE in units [erg/cm2/s/keV] such as
∫0infinityFEdE=σ*(Teff)4.
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Acknowledgements:
J. Poutanen, juri.poutanen(at)oulu.fi
(End) V. Suleimanov [Tubingen Univ.], J. Poutanen [Univ. of Oulu] 04-Jan-2011