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eppaurora.spectra.ediss_specfun_int() A

↳ Parent: eppaurora.spectra

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How to fix Long Method Many Parameters

# coding: utf-8
# Copyright (c) 2020 Stefan Bender
#
# This file is part of pyeppaurora.
# pyeppaurora is free software: you can redistribute it or modify
# it under the terms of the GNU General Public License as published
# by the Free Software Foundation, version 2.
# See accompanying LICENSE file or http://www.gnu.org/licenses/gpl-2.0.html.
"""Particle precipitation spectra

Includes variants describing a normalized particle flux,
as well as variants describing a normalized energy flux.
"""

import numpy as np

__all__ = [
	"exp_general",
	"gaussian_general",
	"maxwell_general",
	"pow_general",
	"pflux_exp",
	"pflux_gaussian",
	"pflux_maxwell",
	"pflux_pow",
	"ediss_spec_int",
	"ediss_specfun_int",
]


# General normalized spectra, standard distributions
def exp_general(en, en_0=10.):
	r"""Exponential number flux spectrum as in Aksnes et al., 2006 [0]

	Defined according to Aksnes et al., JGR 2006, Eq. (1),
	normalized to unit number flux, i.e.
	:math:`\int_0^\infty \phi(E) \text{d}E = 1`.

	Parameters
	----------
	en: float or array_like (N,)
		Energy in [keV]
	en_0: float, optional
		Characteristic energy in [keV] of the distribution.
		Default: 10 keV

	Returns
	-------
	phi: float or array_like (N,)
		Normalized differential hemispherical number flux at `en` in [keV-1 cm-2 s-1]
		([keV] or scaled by 1 keV-2 cm-2 s-1, e.g. ).
	"""
	return 1. / en_0 * np.exp(-en / en_0)


def gaussian_general(en, en_0=10., w=1.):
	r"""Gaussian number flux spectrum as in Fang2008 [1]

	Standard normal distribution with mu = en_0 and sigma = w / sqrt(2)
	for use in Fang et al., JGR 2008, Eq. (1).
	Almost normalized to unit number flux, i.e.
	:math:`\int_0^\infty \phi(E) \text{d}E = 1`
	(ignoring the negative tail).

	Parameters
	----------
	en: float or array_like (N,)
		Energy in [keV]
	en_0: float, optional
		Characteristic energy in [keV], i.e. mode of the distribution.
		Default: 10 keV
	w: float, optional
		Width of the Gaussian distribution, in [keV].

	Returns
	-------
	phi: float or array_like (N,)
		Normalized differential hemispherical number flux at `en` in [keV-1 cm-2 s-1]
		([keV] or scaled by 1 keV-2 cm-2 s-1, e.g.).
	"""
	return 1. / np.sqrt(np.pi * w**2) * np.exp(-(en - en_0)**2 / w**2)


def maxwell_general(en, en_0=10.):
	r"""Maxwell number flux spectrum as in Fang2008 [1]

	Defined in Fang et al., JGR 2008, Eq. (1),
	normalized to :math:`\int_0^\infty \phi(E) \text{d}E = 1`.

	Parameters
	----------
	en: float or array_like (N,)
		Energy in [keV]
	en_0: float, optional
		Characteristic energy in [keV], i.e. mode of the distribution.
		Default: 10 keV

	Returns
	-------
	phi: float or array_like (N,)
		Normalized differential hemispherical number flux at `en` in [keV-1 cm-2 s-1]
		([keV] or scaled by 1 keV-2 cm-2 s-1, e.g.).
	"""
	return en / en_0**2 * np.exp(-en / en_0)


def pow_general(en, en_0=10., gamma=-3., het=True):
	r"""Power-law number flux spectrum as in Strickland1993 [3]

	Defined e.g. in Strickland et al., 1993,
	normalized to unit particle flux:
	:math:`\int_{E_0}^\infty \phi(E) \text{d}E = 1`
	for the high-energy tail version, and
	:math:`\int_0^{E_0} \phi(E) \text{d}E = 1`
	for the low-energy tail version.

	Parameters
	----------
	en: float or array_like (N,)
		Energy in [keV]
	en_0: float, optional
		Characteristic energy in [keV], i.e. mode of the distribution.
		Default: 10 keV
	gamma: float, optional
		Exponent of the power-law distribution, in [keV].
	het: bool, optional
		Return a high-energy tail (het, default: true) for en > en_0,
		or low-energy tail (false) for en < en_0.
		Adjusts the normalization accordingly.

	Returns
	-------
	phi: float or array_like (N,)
		Normalized differential hemispherical number flux at `en` in [keV-1 cm-2 s-1]
		([keV] or scaled by 1 keV-2 cm-2 s-1, e.g.).
	"""
	spec = (gamma + 1) / en_0 * (en / en_0)**gamma
	if het:
		spec[en < en_0] = 0.
		return -spec
	spec[en > en_0] = 0.
	return spec


def pflux_exp(en, en_0=10.):
	r"""Exponential particle flux spectrum

	Normalized to unit energy flux:
	:math:`\int_0^\infty \phi(E) E \text{d}E = 1`.

	Parameters
	----------
	en: float or array_like (N,)
		Energy in [keV]
	en_0: float, optional
		Characteristic energy in [keV], i.e. mode of the distribution.
		Default: 10 keV.

	Returns
	-------
	phi: float or array_like (N,)
		Hemispherical differential particle flux at `en` in [keV-1 cm-2 s-1]
		([kev-2] scaled by unit energy flux).
	"""
	return exp_general(en, en_0=en_0) / en_0


def pflux_gaussian(en, en_0=10., w=1):
	r"""Gaussian particle flux spectrum

	Defined in Fang et al., JGR 2008, Eq. (1).

	Normalized to :math:`\int_0^\infty \phi(E) E \text{d}E = 1`.
	(ignoring the negative tail).
	Parameters
	----------
	en: float or array_like (N,)
		Energy in [keV]
	en_0: float, optional
		Characteristic energy in [keV], i.e. mode of the distribution.
		Default: 10 keV.

	Returns
	-------
	phi: float or array_like (N,)
		Hemispherical differential particle flux at `en` in [keV-1 cm-2 s-1]
		([kev-2] scaled by unit energy flux).
	"""
	return gaussian_general(en, en_0=en_0, w=w) / en_0


def pflux_maxwell(en, en_0=10.):
	r"""Maxwell particle flux spectrum as in Fang2008 [1]

	Defined in Fang et al., JGR 2008, Eq. (1).
	The total precipitating energy flux is fixed to 1 keV cm-2 s-1,
	multiply by Q_0 [keV cm-2 s-1] to scale the particle flux.

	Normalized to :math:`\int_0^\infty \phi(E) E \text{d}E = 1`.

	Parameters
	----------
	en: float or array_like (N,)
		Energy in [keV]
	en_0: float, optional
		Characteristic energy in [keV], i.e. mode of the distribution.
		Default: 10 keV.

	Returns
	-------
	phi: float or array_like (N,)
		Hemispherical differential particle flux at `en` in [keV-1 cm-2 s-1]
		([kev-2] scaled by unit energy flux).
	"""
	return 0.5 / en_0 * maxwell_general(en, en_0)


def pflux_pow(en, en_0=10., gamma=-3., het=True):
	r"""Power-law particle flux spectrum

	Defined e.g. in Strickland et al., 1993.
	Normalized to :math:`\int_{E_0}^\infty \phi(E) E \text{d}E = 1`
	for the high-energy tail version, and to
	:math:`\int_0^{E_0} \phi(E) E \text{d}E = 1`
	for the low-energy tail version.

	Parameters
	----------
	en: float or array_like (N,)
		Energy in [keV]
	en_0: float, optional
		Characteristic energy in [keV], i.e. mode of the distribution.
		Default: 10 keV
	gamma: float, optional
		Exponent of the power-law distribution, in [keV].
	het: bool, optional (default True)
		Return a high-energy tail (true) for en > en_0,
		or low-energy tail (false) for en < en_0.
		Adjusts the normalization accordingly.

	Returns
	-------
	phi: float or array_like (N,)
		Hemispherical differential particle flux at `en` in [keV-1 cm-2 s-1]
		([kev-2] scaled by unit energy flux).
	"""
	return (gamma + 2) / (gamma + 1) / en_0 * pow_general(en, en_0=en_0, gamma=gamma, het=het)


def ediss_spec_int(
	ens,
	dfluxes,
	scale_height,
	rho,
	func,
	axis=-1,
	func_kws=None,
):
	r"""Integrate over a given energy spectrum

	Integrates a mono-energetic parametrization `q`, e.g. from Fang et al., 2010
	using the given differential particle spectrum `phi`:

	:math:`\int_\text{spec} \phi(E) q(E, Q) E \text{d}E`

	This function uses the differential spectrum evaluated at the given energy bins.

	Parameters
	----------
	ens: array_like (M,...)
		Central (bin) energies of the spectrum
	dfluxes: array_like (M,...)
		Differential particle fluxes in the given bins
	scale_height: array_like (N,...)
		The atmospheric scale heights
	rho: array_like (N,...)
		The atmospheric densities, corresponding to the
		scale heights.
	func: callable
		Mono-energetic energy dissipation function to integrate.
	axis: int, optional
		The axis to use for integration, default: -1 (last axis).
	func_kws: dict-like, optional
		Optional keyword arguments to pass to the mono-energetic
		energy dissipation function. Default: `None`

	Returns
	-------
	en_diss: array_like (N)
		The dissipated energy profiles [keV].

	See Also
	--------
	ediss_specfun_int
	"""
	ens = np.atleast_1d(ens)
	dfluxes = np.atleast_1d(dfluxes)
	scale_height = np.atleast_1d(scale_height)
	rho = np.atleast_1d(rho)
	func_kws = func_kws or dict()
	ediss = func(
		ens[None, None, :],
		dfluxes,
		scale_height[..., None],
		rho[..., None],
		**func_kws,
	)
	return np.trapz(ediss * ens, ens, axis=axis)


def ediss_specfun_int(
	energy,
	flux,
	scale_height,
	rho,
	ediss_func,
	ediss_kws=None,
	bounds=(0.1, 300.),
	nstep=128,
	spec_fun=pflux_maxwell,
	spec_kws=None,
):
	"""Integrate mono-energetic parametrization over a spectrum

	Integrates the mono-energetic parametrization over a spectrum given by a
	functional dependence with characteristic energy `energy` and total energy
	flux `flux`.

	Parameters
	----------
	energy: float or array_like (M,...)
		Characteristic energy E_0 [keV] of the spectral distribution.
	flux: float or array_like (M,...)
		Integrated energy flux Q_0 [keV / cm² / s¹]
	scale_height: float or array_like (N,...)
		The atmospheric scale heights [cm].
	rho: float or array_like (N,...)
		The atmospheric mass density [g / cm³]
	ediss_func: callable
		Mono-energetic energy dissipation function to integrate.
	ediss_kws: dict-like, optional
		Optional keyword arguments to pass to the mono-energetic
		energy dissipation function. Default: `None`
	bounds: tuple, optional
		(min, max) [keV] of the integration range to integrate the Maxwellian.
		Make sure that this is appropriate to encompass the spectrum.
		Default: (0.1, 300.)
	nsteps: int, optional
		Number of integration steps, default: 128.
	spec_func: callable, optional, default :func:`pflux_maxwell`
		Spectral shape function, choices are:
		* :func:`pflux_exp` for a exponential spectrum
		* :func:`pflux_gaussian` for a Gaussian shaped spectrum
		* :func:`pflux_maxwell` for a Maxwellian shaped spectrum
		* :func:`pflux_pow` for a power-law
	spec_kws: dict-like, optional
		Optional keyword arguments to pass to the spectral function
		Default: `None`

	Returns
	-------
	en_diss: array_like (M,N)
		The dissipated energy profiles [keV].

	See Also
	--------
	ediss_spec_int
	"""
	energy = np.asarray(energy)
	flux = np.asarray(flux)
	bounds_l10 = np.log10(bounds)
	ens = np.logspace(*bounds_l10, num=nstep)
	ensd = np.reshape(ens, (-1,) + (1,) * energy.ndim)
	spec_kws = spec_kws or dict()
	# "overwrite" the characteristic energy
	spec_kws["en_0"] = energy.T
	dflux = flux.T * spec_fun(ensd, **spec_kws)
	return ediss_spec_int(
		ens, dflux.T, scale_height, rho, ediss_func,
		axis=-1, func_kws=ediss_kws,
	)


1			# coding: utf-8
2			# Copyright (c) 2020 Stefan Bender
3			#
4			# This file is part of pyeppaurora.
5			# pyeppaurora is free software: you can redistribute it or modify
6			# it under the terms of the GNU General Public License as published
7			# by the Free Software Foundation, version 2.
8			# See accompanying LICENSE file or http://www.gnu.org/licenses/gpl-2.0.html.
9			"""Particle precipitation spectra
10
11			Includes variants describing a normalized particle flux,
12			as well as variants describing a normalized energy flux.
13			"""
14
15			import numpy as np
16
17			__all__ = [
18			"exp_general",
19			"gaussian_general",
20			"maxwell_general",
21			"pow_general",
22			"pflux_exp",
23			"pflux_gaussian",
24			"pflux_maxwell",
25			"pflux_pow",
26			"ediss_spec_int",
27			"ediss_specfun_int",
28			]
29
30
31			# General normalized spectra, standard distributions
32			def exp_general(en, en_0=10.):
33			r"""Exponential number flux spectrum as in Aksnes et al., 2006 [0]
34
35			Defined according to Aksnes et al., JGR 2006, Eq. (1),
36			normalized to unit number flux, i.e.
37			:math:`\int_0^\infty \phi(E) \text{d}E = 1`.
38
39			Parameters
40			----------
41			en: float or array_like (N,)
42			Energy in [keV]
43			en_0: float, optional
44			Characteristic energy in [keV] of the distribution.
45			Default: 10 keV
46
47			Returns
48			-------
49			phi: float or array_like (N,)
50			Normalized differential hemispherical number flux at `en` in [keV-1 cm-2 s-1]
51			([keV] or scaled by 1 keV-2 cm-2 s-1, e.g. ).
52			"""
53			return 1. / en_0 * np.exp(-en / en_0)
54
55
56			def gaussian_general(en, en_0=10., w=1.):
57			r"""Gaussian number flux spectrum as in Fang2008 [1]
58
59			Standard normal distribution with mu = en_0 and sigma = w / sqrt(2)
60			for use in Fang et al., JGR 2008, Eq. (1).
61			Almost normalized to unit number flux, i.e.
62			:math:`\int_0^\infty \phi(E) \text{d}E = 1`
63			(ignoring the negative tail).
64
65			Parameters
66			----------
67			en: float or array_like (N,)
68			Energy in [keV]
69			en_0: float, optional
70			Characteristic energy in [keV], i.e. mode of the distribution.
71			Default: 10 keV
72			w: float, optional
73			Width of the Gaussian distribution, in [keV].
74
75			Returns
76			-------
77			phi: float or array_like (N,)
78			Normalized differential hemispherical number flux at `en` in [keV-1 cm-2 s-1]
79			([keV] or scaled by 1 keV-2 cm-2 s-1, e.g.).
80			"""
81			return 1. / np.sqrt(np.pi * w*2) np.exp(-(en - en_0)2 / w2)
82
83
84			def maxwell_general(en, en_0=10.):
85			r"""Maxwell number flux spectrum as in Fang2008 [1]
86
87			Defined in Fang et al., JGR 2008, Eq. (1),
88			normalized to :math:`\int_0^\infty \phi(E) \text{d}E = 1`.
89
90			Parameters
91			----------
92			en: float or array_like (N,)
93			Energy in [keV]
94			en_0: float, optional
95			Characteristic energy in [keV], i.e. mode of the distribution.
96			Default: 10 keV
97
98			Returns
99			-------
100			phi: float or array_like (N,)
101			Normalized differential hemispherical number flux at `en` in [keV-1 cm-2 s-1]
102			([keV] or scaled by 1 keV-2 cm-2 s-1, e.g.).
103			"""
104			return en / en_0*2 np.exp(-en / en_0)
105
106
107			def pow_general(en, en_0=10., gamma=-3., het=True):
108			r"""Power-law number flux spectrum as in Strickland1993 [3]
109
110			Defined e.g. in Strickland et al., 1993,
111			normalized to unit particle flux:
112			:math:`\int_{E_0}^\infty \phi(E) \text{d}E = 1`
113			for the high-energy tail version, and
114			:math:`\int_0^{E_0} \phi(E) \text{d}E = 1`
115			for the low-energy tail version.
116
117			Parameters
118			----------
119			en: float or array_like (N,)
120			Energy in [keV]
121			en_0: float, optional
122			Characteristic energy in [keV], i.e. mode of the distribution.
123			Default: 10 keV
124			gamma: float, optional
125			Exponent of the power-law distribution, in [keV].
126			het: bool, optional
127			Return a high-energy tail (het, default: true) for en > en_0,
128			or low-energy tail (false) for en < en_0.
129			Adjusts the normalization accordingly.
130
131			Returns
132			-------
133			phi: float or array_like (N,)
134			Normalized differential hemispherical number flux at `en` in [keV-1 cm-2 s-1]
135			([keV] or scaled by 1 keV-2 cm-2 s-1, e.g.).
136			"""
137			spec = (gamma + 1) / en_0 * (en / en_0)**gamma
138			if het:
139			spec[en < en_0] = 0.
140			return -spec
141			spec[en > en_0] = 0.
142			return spec
143
144
145			def pflux_exp(en, en_0=10.):
146			r"""Exponential particle flux spectrum
147
148			Normalized to unit energy flux:
149			:math:`\int_0^\infty \phi(E) E \text{d}E = 1`.
150
151			Parameters
152			----------
153			en: float or array_like (N,)
154			Energy in [keV]
155			en_0: float, optional
156			Characteristic energy in [keV], i.e. mode of the distribution.
157			Default: 10 keV.
158
159			Returns
160			-------
161			phi: float or array_like (N,)
162			Hemispherical differential particle flux at `en` in [keV-1 cm-2 s-1]
163			([kev-2] scaled by unit energy flux).
164			"""
165			return exp_general(en, en_0=en_0) / en_0
166
167
168			def pflux_gaussian(en, en_0=10., w=1):
169			r"""Gaussian particle flux spectrum
170
171			Defined in Fang et al., JGR 2008, Eq. (1).
172
173			Normalized to :math:`\int_0^\infty \phi(E) E \text{d}E = 1`.
174			(ignoring the negative tail).
175			Parameters
176			----------
177			en: float or array_like (N,)
178			Energy in [keV]
179			en_0: float, optional
180			Characteristic energy in [keV], i.e. mode of the distribution.
181			Default: 10 keV.
182
183			Returns
184			-------
185			phi: float or array_like (N,)
186			Hemispherical differential particle flux at `en` in [keV-1 cm-2 s-1]
187			([kev-2] scaled by unit energy flux).
188			"""
189			return gaussian_general(en, en_0=en_0, w=w) / en_0
190
191
192			def pflux_maxwell(en, en_0=10.):
193			r"""Maxwell particle flux spectrum as in Fang2008 [1]
194
195			Defined in Fang et al., JGR 2008, Eq. (1).
196			The total precipitating energy flux is fixed to 1 keV cm-2 s-1,
197			multiply by Q_0 [keV cm-2 s-1] to scale the particle flux.
198
199			Normalized to :math:`\int_0^\infty \phi(E) E \text{d}E = 1`.
200
201			Parameters
202			----------
203			en: float or array_like (N,)
204			Energy in [keV]
205			en_0: float, optional
206			Characteristic energy in [keV], i.e. mode of the distribution.
207			Default: 10 keV.
208
209			Returns
210			-------
211			phi: float or array_like (N,)
212			Hemispherical differential particle flux at `en` in [keV-1 cm-2 s-1]
213			([kev-2] scaled by unit energy flux).
214			"""
215			return 0.5 / en_0 * maxwell_general(en, en_0)
216
217
218			def pflux_pow(en, en_0=10., gamma=-3., het=True):
219			r"""Power-law particle flux spectrum
220
221			Defined e.g. in Strickland et al., 1993.
222			Normalized to :math:`\int_{E_0}^\infty \phi(E) E \text{d}E = 1`
223			for the high-energy tail version, and to
224			:math:`\int_0^{E_0} \phi(E) E \text{d}E = 1`
225			for the low-energy tail version.
226
227			Parameters
228			----------
229			en: float or array_like (N,)
230			Energy in [keV]
231			en_0: float, optional
232			Characteristic energy in [keV], i.e. mode of the distribution.
233			Default: 10 keV
234			gamma: float, optional
235			Exponent of the power-law distribution, in [keV].
236			het: bool, optional (default True)
237			Return a high-energy tail (true) for en > en_0,
238			or low-energy tail (false) for en < en_0.
239			Adjusts the normalization accordingly.
240
241			Returns
242			-------
243			phi: float or array_like (N,)
244			Hemispherical differential particle flux at `en` in [keV-1 cm-2 s-1]
245			([kev-2] scaled by unit energy flux).
246			"""
247			return (gamma + 2) / (gamma + 1) / en_0 * pow_general(en, en_0=en_0, gamma=gamma, het=het)
248
249
250			def ediss_spec_int(
251			ens,
252			dfluxes,
253			scale_height,
254			rho,
255			func,
256			axis=-1,
257			func_kws=None,
258			):
259			r"""Integrate over a given energy spectrum
260
261			Integrates a mono-energetic parametrization `q`, e.g. from Fang et al., 2010
262			using the given differential particle spectrum `phi`:
263
264			:math:`\int_\text{spec} \phi(E) q(E, Q) E \text{d}E`
265
266			This function uses the differential spectrum evaluated at the given energy bins.
267
268			Parameters
269			----------
270			ens: array_like (M,...)
271			Central (bin) energies of the spectrum
272			dfluxes: array_like (M,...)
273			Differential particle fluxes in the given bins
274			scale_height: array_like (N,...)
275			The atmospheric scale heights
276			rho: array_like (N,...)
277			The atmospheric densities, corresponding to the
278			scale heights.
279			func: callable
280			Mono-energetic energy dissipation function to integrate.
281			axis: int, optional
282			The axis to use for integration, default: -1 (last axis).
283			func_kws: dict-like, optional
284			Optional keyword arguments to pass to the mono-energetic
285			energy dissipation function. Default: `None`
286
287			Returns
288			-------
289			en_diss: array_like (N)
290			The dissipated energy profiles [keV].
291
292			See Also
293			--------
294			ediss_specfun_int
295			"""
296			ens = np.atleast_1d(ens)
297			dfluxes = np.atleast_1d(dfluxes)
298			scale_height = np.atleast_1d(scale_height)
299			rho = np.atleast_1d(rho)
300			func_kws = func_kws or dict()
301			ediss = func(
302			ens[None, None, :],
303			dfluxes,
304			scale_height[..., None],
305			rho[..., None],
306			**func_kws,
307			)
308			return np.trapz(ediss * ens, ens, axis=axis)
309
310
311			def ediss_specfun_int(
312			energy,
313			flux,
314			scale_height,
315			rho,
316			ediss_func,
317			ediss_kws=None,
318			bounds=(0.1, 300.),
319			nstep=128,
320			spec_fun=pflux_maxwell,
321			spec_kws=None,
322			):
323			"""Integrate mono-energetic parametrization over a spectrum
324
325			Integrates the mono-energetic parametrization over a spectrum given by a
326			functional dependence with characteristic energy `energy` and total energy
327			flux `flux`.
328
329			Parameters
330			----------
331			energy: float or array_like (M,...)
332			Characteristic energy E_0 [keV] of the spectral distribution.
333			flux: float or array_like (M,...)
334			Integrated energy flux Q_0 [keV / cm² / s¹]
335			scale_height: float or array_like (N,...)
336			The atmospheric scale heights [cm].
337			rho: float or array_like (N,...)
338			The atmospheric mass density [g / cm³]
339			ediss_func: callable
340			Mono-energetic energy dissipation function to integrate.
341			ediss_kws: dict-like, optional
342			Optional keyword arguments to pass to the mono-energetic
343			energy dissipation function. Default: `None`
344			bounds: tuple, optional
345			(min, max) [keV] of the integration range to integrate the Maxwellian.
346			Make sure that this is appropriate to encompass the spectrum.
347			Default: (0.1, 300.)
348			nsteps: int, optional
349			Number of integration steps, default: 128.
350			spec_func: callable, optional, default :func:`pflux_maxwell`
351			Spectral shape function, choices are:
352			* :func:`pflux_exp` for a exponential spectrum
353			* :func:`pflux_gaussian` for a Gaussian shaped spectrum
354			* :func:`pflux_maxwell` for a Maxwellian shaped spectrum
355			* :func:`pflux_pow` for a power-law
356			spec_kws: dict-like, optional
357			Optional keyword arguments to pass to the spectral function
358			Default: `None`
359
360			Returns
361			-------
362			en_diss: array_like (M,N)
363			The dissipated energy profiles [keV].
364
365			See Also
366			--------
367			ediss_spec_int
368			"""
369			energy = np.asarray(energy)
370			flux = np.asarray(flux)
371			bounds_l10 = np.log10(bounds)
372			ens = np.logspace(*bounds_l10, num=nstep)
373			ensd = np.reshape(ens, (-1,) + (1,) * energy.ndim)
374			spec_kws = spec_kws or dict()
375			# "overwrite" the characteristic energy
376			spec_kws["en_0"] = energy.T
377			dflux = flux.T * spec_fun(ensd, **spec_kws)
378			return ediss_spec_int(
379			ens, dflux.T, scale_height, rho, ediss_func,
380			axis=-1, func_kws=ediss_kws,
381			)
382

st-bender / pyeppaurora

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eppaurora.spectra.ediss_specfun_int() A

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