Star¶
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class
libra.starspots.
Star
(spots=None, u1=0.4987, u2=0.1772, r=1, radius_threshold=0.1, rotation_period=<Quantity 25. d>)[source] [edit on github]¶ Bases:
object
Object defining a star.
The star is assumed to have stellar inclination 90 deg (equator-on).
Parameters: u1 : float (optional)
Quadratic limb-darkening parameter, linear term
u2 : float (optional)
Quadratic limb-darkening parameter, quadratic term
r : float (optional)
Stellar radius (default is unity)
radius_threshold : float (optional)
If all spots are smaller than this radius, use the analytic solution to compute the stellar centroid, otherwise use the numerical solution.
spots : list (optional)
List of spots on this star.
rotation_period :
Quantity
Stellar rotation period [default = 25 d].
contrast : float (optional)
Spot contrast relative to photosphere. Default is
c=0.7
Methods Summary
derotate
()flux
(times[, t0])Compute flux at times
as the star rotates.fractional_flux
(times[, t0])Compute stellar flux as a fraction of the unspotted stellar flux at times
as the star rotates.limb_darkening
(r)Compute the intensity at radius r
for quadratic limb-darkening law with parametersStar.u1, Star.u2
.limb_darkening_normed
(r)Compute the normalized intensity at radius r
for quadratic limb-darkening law with parametersStar.u1, Star.u2
.plot
([n, ax])Plot a 2D projected schematic of the star and its spots. rotate
(angle)Rotate the star, by moving the spots. spotted_area
(times[, t0])Compute flux at times
as the star rotates.with_k296_spot_distribution
()with_trappist1_spot_distribution
()Methods Documentation
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derotate
()[source] [edit on github]¶
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flux
(times, t0=0)[source] [edit on github]¶ Compute flux at
times
as the star rotates.Parameters: times: `~numpy.ndarray`
Times
t0 : float
Reference epoch.
Returns: flux :
ndarray
Fluxes at
times
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fractional_flux
(times, t0=0)[source] [edit on github]¶ Compute stellar flux as a fraction of the unspotted stellar flux at
times
as the star rotates.Parameters: times: `~numpy.ndarray`
Times
t0 : float
Reference epoch.
Returns: flux :
ndarray
Fluxes at
times
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limb_darkening
(r)[source] [edit on github]¶ Compute the intensity at radius
r
for quadratic limb-darkening law with parametersStar.u1, Star.u2
.Parameters: r : float or
ndarray
Stellar surface position in radial coords on (0, 1)
Returns: intensity : float
Intensity in un-normalized units
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limb_darkening_normed
(r)[source] [edit on github]¶ Compute the normalized intensity at radius
r
for quadratic limb-darkening law with parametersStar.u1, Star.u2
.Parameters: r : float or
ndarray
Stellar surface position in radial coords on (0, 1)
Returns: intensity : float
Intensity relative to the intensity at the center of the disk.
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plot
(n=3000, ax=None)[source] [edit on github]¶ Plot a 2D projected schematic of the star and its spots.
Parameters: ax :
Axes
Axis object to draw the plot on
n : int
Number of pixels per side in the image.
Returns: ax :
Axes
Matplotlib axis object, with the new plot on it.
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rotate
(angle)[source] [edit on github]¶ Rotate the star, by moving the spots.
Parameters: angle : Quantity
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spotted_area
(times, t0=0)[source] [edit on github]¶ Compute flux at
times
as the star rotates.Parameters: times: `~numpy.ndarray`
Times
t0 : float
Reference epoch.
Returns: area :
ndarray
Area covered by spots at
times
[Hem]
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classmethod
with_k296_spot_distribution
()[source] [edit on github]¶
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classmethod
with_trappist1_spot_distribution
()[source] [edit on github]¶
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