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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
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:
FileName Lrecl Records Explanations
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
Note on tablea2.dat: 360 models of neutron star atmospheres.
Byte-by-byte Description of file: set.dat
Bytes Format Units Label Explanations
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)
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Set [1/18] Set number 4- 8 F5.3 --- l Relative luminosity L/L_edd_ (1) 10- 14 F5.3 keV Teff Effective temperature 16- 20 F5.3 --- fc1 Color correction factor f_c,1_ (2) 22- 26 F5.3 --- fc2 Color correction factor f_c,2_ (2) 28- 32 F5.3 --- fc3 Color correction factor f_c,3_ (2) 34- 38 F5.3 --- fc4 Color correction factor f_c,4_ (2) 40- 44 F5.3 --- fc5 Color correction factor f_c,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
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.
Byte-by-byte Description of file: tablea2.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Set Set number 9- 18 E10.5 keV E Photon energy 22- 31 E10.5 mW/m2/keV F(001) Flux F_E_ for l=0.001 (1) 35- 44 E10.5 mW/m2/keV F(003) Flux F_E_ for l=0.003 (1) 48- 57 E10.5 mW/m2/keV F(010) Flux F_E_ for l=0.01 (1) 61- 70 E10.5 mW/m2/keV F(030) Flux F_E_ for l=0.03 (1) 74- 83 E10.5 mW/m2/keV F(050) Flux F_E_ for l=0.05 (1) 87- 96 E10.5 mW/m2/keV F(070) Flux F_E_ for l=0.07 (1) 100-109 E10.5 mW/m2/keV F(100) Flux F_E_ for l=0.1 (1) 113-122 E10.5 mW/m2/keV F(150) Flux F_E_ for l=0.15 (1) 126-135 E10.5 mW/m2/keV F(200) Flux F_E_ for l=0.2 (1) 139-148 E10.5 mW/m2/keV F(300) Flux F_E_ for l=0.3 (1) 152-161 E10.5 mW/m2/keV F(400) Flux F_E_ for l=0.4 (1) 165-174 E10.5 mW/m2/keV F(500) Flux F_E_ for l=0.5 (1) 178-187 E10.5 mW/m2/keV F(600) Flux F_E_ for l=0.6 (1) 191-200 E10.5 mW/m2/keV F(700) Flux F_E_ for l=0.7 (1) 204-213 E10.5 mW/m2/keV F(750) Flux F_E_ for l=0.75 (1) 217-226 E10.5 mW/m2/keV F(800) Flux F_E_ for l=0.8 (1) 230-239 E10.5 mW/m2/keV F(850) Flux F_E_ for l=0.85 (1) 243-252 E10.5 mW/m2/keV F(900) Flux F_E_ for l=0.9 (1) 256-265 E10.5 mW/m2/keV F(950) Flux F_E_ for l=0.95 (1) 269-278 E10.5 mW/m2/keV F(980) Flux F_E_ for l=0.98 (1)
Note (1): Values of the flux FE in units [erg/cm2/s/keV] such as ∫0infinityFEdE=σ*(Teff)4.
Acknowledgements: J. Poutanen, juri.poutanen(at)oulu.fi
(End) V. Suleimanov [Tubingen Univ.], J. Poutanen [Univ. of Oulu] 04-Jan-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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