Magnetic H EOS: interpolation

	EOS and effective opacities for magnetic neutron stars Interpolating program
Neutron Star Group	[Magnetic H EOS Main page]

Description

This Fortran program interpolates thermodynamic functions and Rosseland opacities (for propagation of radiation parallel and perpendicular to the magnetic field) across the tables which are read from the files hmm*.dat (for 10.5 < lg B < 11.9), hmag*.dat (for 11.9 < lg B < 13.5), or hmn*.dat (for lg B>13.5). Consequently, these files must be in current directory when you run the code. You can get them here. However, if you consider only ordinary strong fields (lgB<13.5), it is sufficient to have only files hmag*.dat in your directory. Similarly, if you are interested only in superstrong fields (lgB>13.5), it is sufficient to have only hmn*.dat; and for treating only moderately strong fields (lg B < 11.9) it is sufficient to have only hmm*.dat.

The first (MAIN) routine is commented-out. If uncommented and compiled, it displays the value of a specified thermodynamic function of opacity on terminal. As is, the file can be linked with another package. Format of usage:

call HMINTER(BLG,TLG,RLG,Kout,OUTPUT,Kret)

Input parameters:

BLG=lg(B) - magnetic field logarithm,
TLG=lg(T) - temperature logarithm,
RLG=lg(R) - logarithm of the astrophysical density parameter,
Kout - corresponds to the desired quantity to be calculated (see below).

Output:

OUTPUT - an interpolated quantity,
Kret - performance indicator, equal to 0 if the interpolation was done normally, and -1 otherwise (for instance, if the input falls out of the tabulated ranges of B, T, and R).

The meaning of OUTPUT depends on Kout as follows:

Kout	OUTPUT	Meaning
1	PLG	lg(P/bar)
2	PNkT	PV/(NkT), where N is number of protons (free and bound)
3	UNkT	U/(NkT)
4	ENTROPY	S/(Nk)
5	CVREL	C_V/Nk
6	CHIT	(d log P/d log T)_V
7	CHIR	-(d log P/d log V)_T
8	FHOPT	"true" ("optical") atomic fraction
9	FHOPT0	true ground-state atomic fraction
10	FH2OPT2	number of H₂ molecules divided by N
11	FCLUST	the fraction of protons comprised in clusters
12	ROSLONG	lg(K0), K0 is the effective Rosseland mean opacity [cm²/g] for radiative transport along B
13	ROSTRAN	lg(K1) - the same but perpendicular to B

Notations for the OUTPUT are the same as in the Tables of data.

Download hminter.f

separation line

[Top of this page] [Magnetic H EOS Main page] [Neutron Star Group] [Department of Theoretical Astrophysics] [Ioffe Institute]

Page design and maintenance by Alexander Potekhin (palex@astro.ioffe.ru). Remarks are always welcome.
Page created on May 30, 2002. last updated on October 19, 2014.