This page hosts the client/server porting of the magnetospheric/exospheric model by
Mura et al [2005]
. The model simulates ions and neutrals of various species and from different sources. Please insert the simulation parameter below, then press the [RUN] button at the bottom of the page. You will receive an E-mail with the simulation results. The simulation will take few minutes or several hours, depending on the simulation complexity.
Acknowledgments:
These activities have been partly funded by the Sun Planet Interactions Digital Environment on Request (SPIDER) Virtual Activity of the Europlanet 2024 Research Infrastucture funded by the European Union Horizon 2020 research and innovation programme under grant agreement No 871149.
Some useful templates:
Go to the
full model
, with all options
Mercury
Sodium exosphere released by photon and thermal desorption
Sodium and Oxygen sputtering from Solar wind
Ion sputtering detected by ELENA instrument
Proton backscattering detected by ELENA instrument
Exoplanets
CoRoT7b planet, sodium exosphere
, with exobase temperature = 2500 K, exobase height = 200 km
CoRoT7b -like planet, sodium exosphere
, with exobase temperature = 10000 K, exobase height = 1 planetary radius
Other
Generic body, Ion sputtering detected by ELENA instrument
Europa, Ion sputtering from Jovian plasma
Your E-mail address, where you'll receive the output:
Enter a description for the simulation:
See an example
Geometrical parameters
Planetary radius (m):
Planetary mass (kg):
Haphelion (AU, from the main body it is orbiting around):
Perihelion (AU, from the main body it is orbiting around):
Mass of Sun, star or planet (if it is a satellite) (kg):
Radius of Sun, star or planet (if it is a satellite) (m):
Planet true anomaly angle (in deg):
Photon flux of the star @ 1AU :
Mean distance from star :
Thermical inputs have been disabled. [
Go to the
full model
to set them
]
Magnetic field parameters
Corrective parameter
: radius between Earth and planet magnetospheres size, expressed in the rispective planetary radii. For Mercury, as an example, this value is usually between 6 and 7, as in Siscoe [1975];
Bx, By, Bz
: upstream Interplanetary magnetic field, in nTesla;
Model number
: two models are available:
Tsyganenko [1996] (1)
and
Luhman-Fresnel [1979] (2)
;
Dipole moment (T m
3
):
Harris sheet magnetic field (T):
Harris sheet thickness (m):
Dipole shift (m):
KP index:
S/W velocity (km/s):
S/W density (cm
-3
):
DST index:
Corrective parameter:
Model number (see above):
Bx (nT):
By (nT):
Bz (nT):
Electric field paramenter
The electric field is calculated by assuming that the surface of the planet has an electric potential similar to that of
Volland [1978]
. The electric potential in any other point of the space is calculated by assuming that any magnetic field line is equi-potential. However, since this evalutation could be very slow, the calculated electric potential is stored in a 3D grid of size
[nx, ny, nz]
. The boudaries of this grid are
X1-X2, Y1-Y2, Z1-Z2
, in planetary radii. The potential in any point of the space is hence calculated by linear interpolation between nearest grid vertexes values.
It is possible to chance the strenght of the electric field by changing the cross-tail
potential drop
(in Volts, logaritmic scale).
The last parameters is needed if the Magnetic field model is not symmetric with respect to the
y
axis. In this case the polar caps do not fit with the Volland field shape. It is hence possible to re-calculate the potential inside polar caps with a Gauss-Seidel iterative method (uses Laplace equation). In most cases, use parameter=1.
Grid size and density
X1 / X2 (Rm):
, nx:
Y1 / Y2 (Rm):
, ny:
Z1 / Z2 (Rm):
, nz:
Physical parameters
Potential drop (V) :
Model number (1: Pure Volland 2: Gauss-Seidel) :
Sources
This matrix is needed to specify which physical sources are included in the model. It is possible to include an unlimited number of sources/species at the same time. Add a line for each source process (at least one line). The first value is the code of the source process, according to the following list:
Solar wind at the magnetopause
(SW, code 1)
;
Photo-stimulated desorption, energy distribution as in Wurz and Lammer (2003)
(PSD, code 2)
;
Photo-stimulated desorption, energy distribution using a maxwellian
(PSD, code 12)
;
Thermal desorption
(TD, code 3)
;
Thermal release from the exobase
(TE, code 13)
;
Micro-meteoritic sputtering
(MSP, code 6)
;
Plasma distribution, isotropic
(UPP, code 21)
;
Plasma distribution, collimated
(PPP, code 22)
;
After the code of the source process, add some parameters following this table:
1 (Solar Wind)
unused
upstrem density (cm
-3
)
upstream velocity (km/s)
upstream temperature(K)
unused
unused
2 (Photon desorption)
Atomic Number
beta parameter
distribution temperature (K)
cross section (m
-2
)
parameter(*)
parameter(**)
12 (Photon desorption)
Atomic Number
unused
Temperature
cross section (m
-2
)
unused
unused
3 (Thermal Desorption)
Atomic Number
binding energy (eV)
vibration frequency (s
-1
)
unused
unused
unused
13 (from exobase)
Atomic Number
binding energy (eV)
vibration frequency (s
-1
)
unused
unused
unused
6 (micrometeroids)
Atomic Number
Temperature(K)
Mean mass flux (g*cm
-2
s
-1
)
unused
unused
unused
21 (isotropic plasma)
Atomic Number
Charge (e)
Mean energy (eV)
energy widht (eV)
flux (cm
-2
s
-1
)
unused
22 (collimated plasma)
Atomic Number
Charge (e)
Mean energy (eV)
energy widht (eV)
flux (cm
-2
s
-1
)
unused
1 0 60.0 450 2.0E5 0 0 [1=Solar wind; 0=PAD; 60=density; 450=velocity; 2E5=temperature; 0,0=PAD]
* this parameter (n) controls the dependance of the flux vs solar-zenith angle (angle from subsolar point). The function is usually cos(angle)
n
, where n=1.
** this parameter (n) controls the dependance of the flux vs direction angle (angle from the vertical). The function is usually cos(angle)
n
, where n=2.
Sputtering (4, 5) are simulations of the effects of H+ sputtering without simulating H+ trejectories themselves (faster simulation). In the case (
4 HSP
) the flux of H+ over the planetary surface has been simulated in an average case (see
Mura et al, [2005]
), and then stored. In this way, there is no need to simulate H+ to obtain sputtering. The case (
5 HSP
) the H+ flux over the dayside surface is calculated as
F=Fup*cos(a)
where Fup is the unperturbed, upstream S/W flux and a is the angle from the subsolar point.
Examples:
1 0 60.0 450 5000.0 0 0 Solar wind protons entering from magnetopause 2 11 0.7 600 1.E-25 1 2 Sodium Photo-Stimulated Des. 12 11 0.7 1500 1.E-25 1 2 Sodium Photo-Stimulated Des., Maxwellian source 3 11 1.85 1.E13 0 0 0 Sodium Thermal Des. 6 11 4000 6E-15 247 0 0 Micrometeorites extract Sodium
Processes
You can add one or more loss process here. Some of these loss processes also produce a secondary particle (for example, photo-ionization of neutrals produce ions). Add a line for each loss process (at least one line). The first value is the code of the loss process, according to the following list:
Surface ion-sputtering
(SP, code 1)
, i.e. the extraction of a neutral from the surface by any impacting ion;
Photon-ionization
(PI, code 2)
of a neutral, producing an ion in the simulation;
Photon-ionization
(PI, code 12) of a neutral. The resulting ion is not simulated
;
Secondary photon-ionization
(PI, code 22)
of an ion, producing an ion++ in the simulation;
Secondary Photon-ionization
(PI, code 32) of an ion. The resulting ion++ is not simulated
;
Charge-Exchange
(CE, code 3)
between ion and exopsheric neutrals (see
section 4
).
The use of this matrix is similar to the previous one. Add as many lines as you want.
1 (Sputtering)
Atomic number
binding energy (eV)
yield
cosine exponent
2 (PhotoIon.)
Atomic number
unused
lifetime (s)
unused
12 (PhotoIon.)
Atomic number
unused
lifetime (s)
unused
22 (PhotoIon.)
Atomic number
unused
lifetime (s)
unused
32 (PhotoIon.)
Atomic number
unused
lifetime (s)
unused
3 (Charge-Ex.)
Atomic number
unused
unused
unused
5 (Chemic. Sput.)
Atomic number
yield
temperature (K)
unused
6 (Atm. scattering)
Atomic number
unused
unused
unused
25 (Surface scattering)
Atomic number
yield
cosine exponent
unused
1 08 3 0.1 4 [1=Sputtering, 08=Oxygen, 3=binding energy, 0.1=yield, 4=cosine exp.] 1 11 2 0.1 4 [1=Sputtering, 11=Sodium, 2=binding energy, 0.1=yield, 4=cosine exp.]
Examples:
1 11 2 1 4 Sputtering of Sodium by any ion 1 8 4 1 2 Sputtering of Oxygen by any ion 2 11 0 2.E4 0 Sodium photoionization 2 8 0 7.E5 0 Oxygen photoionization
Surface composition and radiation pressure table
Please insert a table of the needed atomic species using this template:
Atomic Number (
Z
)
Surface composition (%)
Radiation Pressure (cm s
-2
)
Radiation pressure should negative, in cm s
-2
; a value =1 indicates that you want the model to calculate the radiation pressurre. Radiation pressure may be calculated by the model for Sodium, Hydrogen or Potassium only. In this case, the radiation pressure is calculated at every time-step, taking into account the doppler effect. Please insert a line for each specied included in the simulation. Please check/modify the parameters...
1 0 1 Hydrogen, with radiation pressure 08 57.7 0 Oxigen, no radiation pressure 11 0.49 1 Sodium, with radiation pressure 19 0.034 1 K, with radiation pressure 20 1.58 -45 Ca, constant radiation pressure 12 16 -0.2 Mg, very weak radiation pressure
Surface composition map inputs have been disabled. [
Go to the
full model
to set them
]
Additional atmospheric parameters have been disabled. [
Go to the
full model
to set them
]
Output: Spherical accumulation grid:
Please specify the 6 boundary values of the grid:
R1
and
R2
: minimum and maximum radius, in planetary radii;
Lat1
and
Lat2
: minimum and maximum latitude, in degrees;
Lon1
and
Lon2
: minimum and maximum longitude, in degrees;
as well as the grid size, in bins (
n-R, n-Lat, n-Lon
)
Radius.
R1 / R2 (rm):
, n-:
Latitude
. Lat 1 / Lat 2 (deg):
, n-:
Longitude
. Lon 1 / Lon 2 (deg):
, n-:
The number of the other dimensions of the accumulation grid are free, and the accumulation matrix will be "sparse" in these dimensions. You can specify a free number of energy channels, atomic number (
Z
) channels, charge channels, and pitch-angle (P.A.) channels. Please use the following template to fill the matrix, and add as many lines as yu like:
Min. Energy
Max. Energy
Min. Z
Max. Z
Min. charge
Max. charge
Min. P.A.
Max. P.A.
Energy channels
Z channels
Charge channels
PA channels
Flag (1=on)
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
Where energies are in "eV", atomic numbers in "Z", charges in "e", pitch angles are in "deg". Some templates have been included below:
.0001 100000 1 100 -1 1 0 180 1 1 1 1 1 [All masses, no energy,mass or pitch angle resolution]
Examples:
.0001 100000 11 11 -1 1 0 180 1 1 1 1 1 [Sodium, all charge states, no energy resolution] .0001 100000 08 08 -1 1 0 180 8 1 1 1 1 [Oxygen, all charge states, with 8 log. channels energy resolution] .0001 100000 1 1 1 1 0 180 12 1 1 1 1 [Protons, charge=1, with 12 log. channels energy resolution]
Output: Cubic accumulation grid
: similar to the spherical one.
X1 / X2 (Rm):
, n-x:
Y1 / Y2 (Rm):
, n-y:
Z1 / Z2 (Rm):
, n-z:
The number of the other dimensions of the accumulation grid are free, and the accumulation matrix will be "sparse" in these dimensions. You can specify a free number of energy channels, atomic number (
Z
) channels, charge channels, and pitch-angle (P.A.) channels. Please use the following template to fill the matrix, and add as many lines as yu like:
Min. Energy
Max. Energy
Min. Z
Max. Z
Min. charge
Max. charge
Min. P.A.
Max. P.A.
Energy channels
Z channels
Charge channels
PA channels
Flag (1=on)
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
...
Where energies are in "eV", atomic numbers in "Z", charges in "e", pitch angles are in "deg". Some templates have been included below:
.0001 100000 1 100 -1 1 0 180 1 1 1 1 1 All masses, charge, energies
Examples:
.0001 100000 11 11 -1 1 0 180 1 1 1 1 1 [Sodium, all charge states, no energy resolution] .0001 100000 08 08 -1 1 0 180 8 1 1 1 1 [Oxygen, all charge states, with 8 log. channels energy resolution] .0001 100000 1 1 1 1 0 180 12 1 1 1 1 [Protons, charge=1, with 12 log. channels energy resolution]
Instrumental simulation parameters have been disabled. [
Go to the
full model
to set them
]
See an example
References
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Barnett, C. F., J. A. Ray, E. Ricci, M. I. Wilker, E. W. McDaniel, E. W. Thomas and H. B. Gilbody, Physics Division: Atomic Data for Controlled Fusion, Oak Ridge National Laboratory, Oak Ridge, Tennessee, February 1977.
Barnett, C. F., Collisions of H, H2, He and Li atoms and ions with atoms and molecules, Atomic Data for Fusion Ser., vol. 1, Rep. ORNL-6086, edited by H. T. Hunter et al., Oak Ridge Nat. Lab., Oak Ridge, Tenn., 1990.
Broadfoot A.L., D.E. Shemanky, and S. Kumar, Mariner 10: Mercury atmosphere, Geophys. Res. Lett., 3, 577, 1976.
Burlaga, L.F., Magnetic fields and plasma in the inner heliosphere: Helios results. Planet. Space Sci. 49, 1619-1627, 2001.
Delcourt, D. C., S. Grimald, F. Leblanc, J.-J. Berthelier, A. Millilo, A. Mura, and S. Orsini, A quantitative model of planetary Na+ contribution to Mercury s magnetosphere, Annales Geophys, 21, 1723 - 1736, 2003.
Goettel K.A., Present bounds on the bulk composition of Mercury: Implications for planetary formation processes. In Mercury, pp. 613-621, (F. Vilas, C.R. Chapman and M.S. Matthews, Eds.) Univ. Arizona Press, Tucson, 1988.
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Grande, M., Investigation of magnetospheric interactions with the Hermean surface, Adv. Space Res., 19 (10), 1609-1614, 1997.
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Kallio, E., and P. Janhunen (b), The response of the hermean magnetosphere to the interplanetary magnetic field, Adv. Space Res., in press, 2003.
Killen, R.M., A.E. Potter, and T.H. Morgan, Spatial Distribution of sodium vapor in the atmosphere of Mercury, Icarus 85, 145-167, 1990.
Killen, R.M., and W-H Ip, The surface-bounded atmosphere of Mercury and the Moon, Reviews of Geophysics, 361, 1999.
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Leblanc, F., and R. E. Johnson, Mercury s sodium exosphere, Icarus 164, 261, 2003
Luhmann, J.G., C.T. Russell, and N.A. Tsyganenko, Disturbances in Mercury s Magnetosphere: Are the Mariner 10 Substorms Simply Driven?, J. Geophys. Res. 103, 9113-9119, 1998.
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Massetti S., S. Orsini, A. Milillo, A. Mura, E. De Angelis, H. Lammer and P. Wurz, Mapping of the cusp plasma precipitation on the surface of Mercury, Icarus, in press, 2003.
McGrath, M. A., Johnson, R. E., and Lanzerotti, L. J.: Sputtering of sodium on the planet Mercury, Nature, 323, 694-696, 1986.
Ness, N.F., K.W. Behannon, R.P. Lepping, and Y.C. Whang. Observations of Mercury s Magnetic field. Icarus 28, 479-488, 1976.
Ogilvie, K.W., J.D. Scudder, V.M. Vasyliunas, R.E. Hartle, and G.L. Siscoe, Observations at the planet Mercury by the plama electron experiment: Mariner 10, J. Geophys Res., 83, 1807-1824, 1977.
Orsini, S., I. A. Daglis, M. Candidi, K. C. Hsieh, S. Livi, and B. Wilken, Model calculation of energetic neutral atoms precipitating at low altitudes, J. Geophys. Res., 99, 13489, 1994.
Orsini, S., A. Milillo, E. De Angelis, A.M. Di Lellis, V. Zanza, and S. Livi, Remote sensing of Mercury s magnetospheric plasma via energetic neutral atoms imaging, Planet. Space Sci., 49, 1659, 2001.
Potter, A.E., and T.H. Morgan, Discovery of Na in the atmosphere of Mercury, Science 229, 651-653, 1985
Potter, A.E. and T.H. Morgan, Sodium and Potassium Atmospheres of Mercury, Planet. Space. Sci., 45, 95-100. 1997.
Roelof, E. C., D. G. Mitchell, and D. J. Williams, Energetic neutral atoms (E 50 keV) from the ring current, IMP 7/8 and ISEE 1, J. Geophys. Res., 90, 10991, 1985.
Sarantos, M., P. H. Reiff, T. W. Hill, R. Killen, A. L. Urquhart, A Bx-interconnected magnetosphere model for Mercury, Planet. Space Sci., 49, 1629-1635, 2001.
Sigmund, P., Theory of Sputtering. I. Sputtering Yield of Amorphous and Polycrystalline Targets Phys. Rev. 184, 383–416, 1969.
Siscoe, G.L., N.F. Ness, and C. M. Yeates, Substorms on Mercury?, J. Geophys Res., 80, 4359-4363, 1975.
Slavin, J.A., J.C.J. Owen, J.E.P. Connerney, and S.P. Christon, Mariner 10 observations of field-aligned currents at Mercury, Planet. Space Sci., 45, 133-141, 1997.
Sprague, A. L., W. J. Schmitt, and R. E. Hill, Mercury: Sodium atmospheric enhancements, radar bright spots and visible surface features, Icarus 136, 60, 1998
Stebbings, R. F., C. H. Smith, and H. Ehrahardt, Charge transfer between Oxygen atoms and O+ and H+ ions, J. Geophys. Res., 69, 2349, 1964.
Spreiter, J. R., Summers, A. L., Alksne, A. Y., Hydromagnetic flow around the magnetosphere. Planet. Space Sci. 14, 223–253, 1966.
Tsyganenko, N. A., Effects of the solar wind conditions on the global magnetospheric configuration as deduced from data-based field models, in Proc.of 3rd International Conference on Substorms (ICS-3). ESA SP-389, 181-185, 1996.
Spreiter, J.R., A.L. Summers, and A.Y. Alksne, Hydromagnetic flow around the magnetosphere. Planet. Space Sci. 14, 223-253, 1966.
Sieveka, E.M., and R.E. Johnson. Ejection of atoms and molecules from Io by plasma-ion impact. Astrophys. J. 287, 418-426, 1984.
Volland, H. A. Models of global electric fields within the magnetosphere, Ann. Geophys., 31, 159-173, 1975
Volland, H.: A model of the magnetospheric convection electric field, J. Geophys. Res., 83, 2695–2699, 1978.
Weins, R.C., D.S. Burnett, W.F. Calaway, C.S. Hansen, K.R., Lykkem and M.L. Pellin, Sputtering products of sodium sulphate: Implications for Io s surface and for sodium bearing molecules in the Io s torus, Icarus, 128, 386-397, 1997
Wurz, P., and H. Lammer, Monte-Carlo Simulation of Mercury s Exosphere, Icarus, 164(1), 1-13, 2003