本文整理汇总了C++中cube::readngrid方法的典型用法代码示例。如果您正苦于以下问题：C++ cube::readngrid方法的具体用法？C++ cube::readngrid怎么用？C++ cube::readngrid使用的例子？那么恭喜您, 这里精选的方法代码示例或许可以为您提供帮助。您也可以进一步了解该方法所在类cube的用法示例。
在下文中一共展示了cube::readngrid方法的1个代码示例，这些例子默认根据受欢迎程度排序。您可以为喜欢或者感觉有用的代码点赞，您的评价将有助于系统推荐出更棒的C++代码示例。
示例1: emissionfromdatacube
cube emissionfromdatacube(cube datacube)
{
// construct the G(T) using CHIANTI tables
int ng=datacube.readngrid();
int nvars=5; // G(T), width, vx, vy, vz
// take the last 3 from datacube
cube emission(nvars, ng);
tgrid grid=datacube.readgrid();
emission.setgrid(grid);
emission.settype(emisscube);
// copy velocity vectors
for (int i=2; i<nvars; i++)
{
tphysvar velcomp=datacube.readvar(i);
emission.setvar(i,velcomp);
};
tphysvar logrho = log10(datacube.readvar(0));
tphysvar T = datacube.readvar(1);
tphysvar logT = log10(T);
// writearray(logT,"empty");
string ion="";// better to be aia for AIA tables this will be checked for correct table [DY]
double lambda0=.0;
double atweight=1;
cube gofttab=readgoftfromchianti(chiantifile,ion,lambda0,atweight);
// fit the G(T) function to the data points
tphysvar fittedgoft=goft(logT,logrho,gofttab);
// calculate the line width at each data point
tphysvar fittedwidth=linefwhm(T,lambda0,atweight);
// calculate the maximum of the emission profile at each grid point
// The emission in the CHIANTItables is calculated with the sun_coronal.abund file
// There are 2 cases:
// - we are doing spectroscopic calculations: the fittedemission should normalised with the alphaconst, and if a different abundance is used, we should renormalise to the new abundance
// - we are doing intensity calculations (for e.g. AIA): the tables are already in the correct units, and the fittedemission needs to only be multiplied with 1.
double normaliseconst=1.;
double abundratio=1.;
if (lambda_pixel>1) // for spectroscopic study
{
cout << "This code is configured to do spectroscopic modelling" << endl;
// tphysvar fittedwidth=linefwhm(T,lambda0,atweight);
normaliseconst=1./alphaconst;
if (abundfile != string("/empty"))
{
ifstream abundfilestream (abundfile);
cout << "Reading abundances from " << abundfile << "... " << flush;
double abundnew=abundfromchianti(abundfilestream, ion);
cout << "Done!" << endl << flush;
istringstream standardabundfile (______chiantitables_sun_coronal_abund_string);
double abundold=abundfromchianti(standardabundfile,ion);
abundratio=abundnew/abundold;
}
}
if (lambda_pixel==1) // for imaging study
{
if (atoi(ion.c_str())!=int(lambda0+0.5))
{// check if it is AIA GOFT table
cout << "GOFT table is not correct!" << endl;
exit(EXIT_FAILURE);
}
fittedwidth=T/T;// =1.0
}
// Spectral modelling: ne^2 [cm^-3] * G(ne,Te) [erg cm^3 s^1] = emis [erg cm^-3 s^-1]
// for integration *[cm] [D.Y 12 Nov 2014]
// AIA modelling: Temperature response function K(ne,Te)[cm^5 DN S^-1]*ne[cm^-3]=emis [DN cm^-1 s^-1];
// for integration *[cm] [D.Y 12 Nov 20
// cout << "normaliseconst" <<normaliseconst << endl;
// cout << "abundratio"<<abundratio<<endl;
tphysvar fittedemission=normaliseconst*abundratio*pow(10.,2.*logrho)*fittedgoft;
fittedemission=fittedemission/fittedwidth;
// load the emission and width into the emission-cube variable
emission.setvar(0,fittedemission);
emission.setvar(1,fittedwidth);
return emission;
};