`irfpy.mars.exosphere`¶

Martian exosphere models.

Several density models for the Martian upper atmosphere.

ISSI2008_SolarMax: Solar max neutral density model for Mars
ISSI2008_SolarMin: Solar min neutral density model for Mars
ZetaChamberlain1963 Synthesis of three implementations of the partition function.

Sample scripts are also available at snippet_mars.exosphere_max, snippet_mars.exosphere_min, snippet_mars.exosphere_demo

class irfpy.mars.exosphere.ISSI2008_SolarMax[source]¶

Bases: object

The neutral upper atmosphere profiles of CO2, O, and H used in the ISSI SWIM model challenge (solar max)

Code author: X.-D. Wang

Height profiles of five species (CO2, hot_O, cold_O, hot_H, cold_H) are obtained. TODO: include the partition function into the solar maximum profiles too.

>>> from irfpy.mars.exosphere import ISSI2008_SolarMax as exosph

>>> co2_250 = exosph.CO2(250)   # CO2 density at 250 km in /cm3.
>>> print('{:.3e}'.format(co2_250))
1.089e+07

>>> oc_250 = exosph.O_cold(250)   # Cold O denisty at 250 km.
>>> print('{:.3e}'.format(oc_250))
1.655e+07

>>> oh_250 = exosph.O_hot(250)   # Hot O density at 250 km.
>>> print('{:.3e}'.format(oh_250))
1.761e+04

>>> hc_250 = exosph.H_cold(250)  # Cold H density at 250 km.
>>> print('{:.3e}'.format(hc_250))
2.923e+01

>>> hh_250 = exosph.H_hot(250)   # Hot H density at 250 km.
>>> print('{:.3e}'.format(hh_250))
2.835e+04

The original models are fed by the MTGCM model. This is an analytical copy obtained by manual scaling the plots in Brain’s presentation. Following are the original texts on http://www.issibern.ch/teams/martianplasma/

Neutral Atmosphere:
All information will be based on results from Steve Bougher’s MTGCM, and published results from Jean-Yves Chaufray for hydrogen densities /?? Reference preferable ??/. The MTGCM was run for Ls=270, F10.7=105 at Mars.

CO2 number density (CO2()):
5.88e18 * exp( -z / 7.00 ) + 3.55e13 * exp( -z / 16.67 )

‘Cold’ O number density (O_cold()):
2.33e13 * exp( -z / 12.27 ) + 2.84e09 * exp( -z / 48.57 )

‘Cold’ H number density (H_cold()):
1e3 * exp[ 9.25e5 * ( 1 / (z+3393.5) - 1/3593.5) ]

Neutral Temperature (?? Not implemented ??):
-161.13 * exp[ -0.5 * ( (z-112.6) / 25.25 )^2 ] + 291.78

Following are the description of the extra hot corona components of hydrogen and oxygen.

Hot corona / Extended exosphere:

‘Hot’ Neutral Hydrogen (H_hot()):
3e4 * exp[ 1.48e4 * ( 1 / (z+3393.5) - 1/3593.5) ]

‘Hot’ Neutral Oxygen (O_hot()):
1.56e4 * exp( -z / 696.9) + 2.92e3 * exp( -z / 2891.) + 5.01e4 * exp( -z / 99.19)

static CO2(z)[source]¶

CO2 density model for solar max at Mars.

Parameters:: z – Altitude in km.
Returns:: CO2 density in /cm3.

static O_cold(z)[source]¶

Cold O density model for solar max at Mars.

Parameters:: z – Altitude in km.
Returns:: Cold O density in /cm3.

static H_cold(z)[source]¶

Cold H density model for solar max at Mars.

Parameters:: z – Altitude in km.
Returns:: Cold H density in /cm3.

static H_hot(z)[source]¶

Hot H density model for solar max at Mars.

Parameters:: z – Altitude in km.
Returns:: Hot H density in /cm3.

static O_hot(z)[source]¶

Hot O density model for solar max at Mars.

Parameters:: z – Altitude in km.
Returns:: Hot O density in /cm3.

class irfpy.mars.exosphere.ISSI2008_SolarMin[source]¶

Bases: object

The neutral upper atmosphere profiles of CO2, O, and H used in the ISSI SWIM model challenge (solar min).

Code author: X.-D. Wang

Height profiles of the number densities for five species (CO2, hot_O, cold_O, hot_H, cold_H) are obtained.

>>> from irfpy.mars.exosphere import ISSI2008_SolarMin as exosph

>>> co2_250 = exosph.CO2(250)   # CO2 density at 250 km in /cm3.
>>> print('{:.3e}'.format(co2_250))
5.950e+05

>>> oc_250 = exosph.O_cold(250)   # Cold O denisty at 250 km.
>>> print('{:.3e}'.format(oc_250))
4.472e+06

>>> oh_250 = exosph.O_hot(250)   # Hot O density at 250 km.
>>> print('{:.3e}'.format(oh_250))
6.599e+03

>>> hc_250 = exosph.H_cold(250)  # Cold H density at 250 km.
>>> print('{:.3e}'.format(hc_250))
1.358e+05

>>> hh_250 = exosph.H_hot(250)   # Hot H density at 250 km.
>>> print('{:.3e}'.format(hh_250))
1.826e+04

The original models are fed by the MTGCM model. This is an analytical copy obtained by manual scaling the plots in Brain’s presentation. Following are the original texts on http://www.issibern.ch/teams/martianplasma/

Neutral Atmosphere:

All information will be based on results from Steve Bougher’s MTGCM, and published results from Jean-Yves Chaufray for hydrogen densities. The MTGCM was run for Ls=270, F10.7 = 34 at Mars.

z is referenced from the Martian surface, in km. Density has units of cm^-3.

CO2 number density:
6.04e18 * exp( -z / 6.98 ) + 1.67e15 * exp( -z / 11.49 )

O number density:
5.85e13 * exp( -z / 10.56 ) + 7.02e09 * exp( -z / 33.97 )

H number density:
1.5e5 * exp[ 25965 * ( 1 / (z+3393.5) - 1/3593.5) ]

Neutral Temperature:
-64.56 * exp[ -0.5 * ( (z-115.7) / 20.14 )^2 ] + 196.95

Following are the description of the extra hot corona components of hydrogen and oxygen.

Neutral Hydrogen (Cold and Hot):
Use the same cold hydrogen profile as before, but now add a hot component.

hot component:
1.9e4 * exp[ 10365 * ( 1 / (z+3393.5) - 1 / 3593.5) ]

Neutral Oxygen (Cold and Hot):
Use the same cold oxygen profile as before, but now add a hot component, supplied by Arnaud Valeille.

hot component:
5.23e3 * exp( -z / 626.2) + 9.76e2 * exp( -z / 2790.) + 3.71e4 * exp( -z / 88.47) ]

R_m = 3376000.0¶

static part_func(r, lam=None, Tc=200, partfun=0)[source]¶

Polynomial implementation of Chamberlain’s partition function zeta. Obselete due to large error for high altitudes.

Parameters:

r – radius from Mars center, in meters
zc – exobase altitude, in meters
hc – scale height at exobase, in meters
partfun – flag to determine what partition function to use. 1 for polynomial, 2 for Chamberlain1963.

Default values (zc=200e3, hc=1176e3) are for the hot hydrogen component: Tc = 500 K, nc = 1.5e4 cm-3 [chaufray2008] :return: (?? Any description ??)

static CO2(z)[source]¶

CO2 density model for solar min at Mars.

Parameters:: z – Altitude in km.
Returns:: CO2 density in /cm3.

static O_cold(z)[source]¶

Cold O density model for solar min at Mars.

Parameters:: z – Altitude in km.
Returns:: Cold O density in /cm3.

static H_cold(z, part=0)[source]¶

Cold H density model for solar min at Mars.

Parameters:

z – Altitude in km.
part – /?? Any description ??/

Returns:

Cold H density in /cm3.

static H_hot(z, part=0)[source]¶

Hot H density model for solar min at Mars.

Parameters:

z – Altitude in km.
part – /?? Any description ??/

Returns:

Hot H density in /cm3.

static O_hot(z)[source]¶

Hot O density model for solar min at Mars.

Parameters:: z – Altitude in km.
Returns:: Hot O density in /cm3.

class irfpy.mars.exosphere.ZetaChamberlain1963[source]¶

Bases: object

Implementation of Chamberlain’s partition function for ballistic, satellite and escape populations.

Code author: X.-D. Wang

<?? More detailed comments if this class is intended to be used by users ??>

G = 6.67408e-11¶

Mars_mass = 6.417e+23¶

mp = 1.67e-27¶

kb = 1.38e-23¶

R_m = 3376000.0¶

lam_c_tab = array([ 1. , 2. , 3. , 4. , 5. , 7.5, 10. , 15. ])¶

lams_full = array([ 0.1, 0.2, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8, 0.9, 1. , 1.1, 1.2, 1.3, 1.4, 1.5, 1.6, 1.7, 1.8, 1.9, 2. , 2.1, 2.2, 2.3, 2.4, 2.5, 2.6, 2.7, 2.8, 2.9, 3. , 3.5, 4. , 4.5, 5. , 5.5, 6. , 6.5, 7. , 7.5, 8. , 8.5, 9. , 9.5, 10. , 11. , 12. , 13. , 14. , 15. ])¶

beta = 5182756824.000002¶

Tcs = array([1449.31678523, 724.65839262, 483.10559508, 362.32919631, 289.86335705, 193.24223803, 144.93167852, 96.62111902])¶

static gam(a, x)[source]¶: UNNORMALIZED Incomplete Gamma function. = scipy.gamma * scipy.gammainc :param a: :param x: :return:

classmethod zeta_chamberlain1963_tab(lam_c_orig)[source]¶

Tabulated Chamberlain’s partition function. Copied from Chamberlain1963, used to verify the analytical implementation. :param lam_c_orig: Original lambda value.

Returns:: zeta values as a function of lambda.

classmethod zeta_bal_shen1963(r, T)[source]¶

Analytical format for the ballistic orbits from Shen 1963, cited by Chamberlain 1963.

Parameters:

r –
T –

Returns:

classmethod zeta_chamberlain1963(r, Tc=200, planetmass=6.417e+23, rc=3597000.0, particlemass=1.67e-27, lam=None)[source]¶

Partition function from Chamberlain 1963, analytical, with 3 types of orbits.

Parameters:

r – Radius of the point of interest, in meter.
Tc – Exobase temperature, in Kelvin. If lam kwarg is set, At least ONE of r and Tc must be scalar.
planetmass – Mass of the planet, in kg. By default Mars.
rc – Radius of the exobase, in meter. By default the Mars exobase at R_m + 200 km.
particlemass – Mass of the interested particles, in kg. By default hydrogen atom, 1 amu.
lam – Input lambda values instead of radius. If lam is input, it must have the same dimension as r.

Returns:

All returned values have same dimension as the array in r or Tc. lam, lambda values for r with exobase temperature Tc: lambda = G * M * m/(kb * Tc * r) lam_c, lambda value for exobase with temperature Tc: lambda_c = G * M * m/(kb * Tc * rc) z_bal, Ballistic orbit zeta function value(s) at radius r with exobase tmperature Tc. Range [0, 1] z_sat, Satellite orbit zeta function. z_esc, Escape orbit zeta function.

`irfpy.mars.exosphere`¶

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`irfpy.mars.exosphere`¶