ivs.roche.local

get_grid(*args, **kwargs)

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Construct a coordinate grid

If you give two resolutions, the first is for theta, the second for phi

Parameters:

args (integer) - one or two integers indicating number of grid points in theta and phi direction
gtype (str) - grid type ('spher' or 'delaunay')

Returns:

theta,phi(,grid)

stitch_grid(theta, phi, *quant, **kwargs)

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Stitch a grid together that was originally defined on 1 quadrant.

We add the three other quandrants.

surface_normals(r, phi, theta, grid, gtype='spher')

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Numerically compute surface normals of a grid (in absence of analytical alternative).

Also computes the surface elements, making surface_elements obsolete.

surface_elements((r, mygrid), (surfnormal_x, surfnormal_y, surfnormal_z), gtype='spher')

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Compute surface area of elements in a grid.

theta,phi must be generated like mgrid(theta_range,phi_range)

usually, the surfnormals are acquired via differentiation of a gravity potential, and is then equal to the *negative* of the local surface gravity.

temperature(surface_gravity, g_pole, T_pole, beta=1.)

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Calculate local temperature.

beta is gravity darkening parameter.

intensity(teff, grav, mu=None, photband='OPEN.BOL')

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Calculate local intensity.

beta is gravity darkening parameter.

projected_intensity(teff, gravity, areas, line_of_sight, photband='OPEN.BOL')

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Compute projected intensity in the line of sight.

gravity is vector directed inwards in the star line of sight is vector.

project(star, view_long=(0,0,0), view_lat=(pi/2,0,0), photband='OPEN.BOL', only_visible=False, plot_sort=False, scale_factor=1.)

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Project and transform coordinates and vectors to align with the line-of-sight.

Parameter star should be a record array containing fields 'teff','gravx', 'gravy','gravz','areas','vx','vy','vz'

and either you suply ('r','theta','phi') or ('x','y','z')

The XY direction is then the line-of-sight, and the YZ plane is the plane of the sky.

An extra column 'projflux' and 'eyeflux' will be added. Projected flux takes care of limb darkening, and projected surface area. Eye flux only takes care of limbdarkening, and should only be used for plotting reasons.

view_long[0] of 0 means looking in the XY line, pi means looking in the YX line. view_lat[0] of pi/2 means edge on, 0 or pi is pole-on.

This function updates all Cartesian coordinates present in the star, but not the polar coordinates! The projected fluxes are added as a field 'projflux' to the returned record array.

If you set 'only_visible' to True, only the information on the visible parts of the star will be contained.

If you set 'plot_sort' to True, the arrays will be returned in a sorted order, where the areas at the back come first. This is especially handy for plotting.

Parameters:

view_long (tuple floats (radians,x,y)) - longitude viewing angle (radians) and coordinate zeropoint
view_lat (tuple floats (radians,x,z)) - inclination viewing angle (radians) and coordinate zeropoint
photband (string) - photometric passband
only_visible (boolean) - flag to return only information on visible surface elements
plot_sort (boolean) - flag to sort the surface elements from back to front
star (numpy record array)

Module local

get_grid(*args, **kwargs)

stitch_grid(theta, phi, *quant, **kwargs)

surface_normals(r, phi, theta, grid, gtype='spher')

surface_elements((r, mygrid), (surfnormal_x, surfnormal_y, surfnormal_z), gtype='spher')

temperature(surface_gravity, g_pole, T_pole, beta=1.)

intensity(teff, grav, mu=None, photband='OPEN.BOL')

projected_intensity(teff, gravity, areas, line_of_sight, photband='OPEN.BOL')

project(star, view_long=(0,0,0), view_lat=(pi/2,0,0), photband='OPEN.BOL', only_visible=False, plot_sort=False, scale_factor=1.)