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Papers by H. Durand-Manterola
AIP Conference Proceedings, 2006
From the models of Titan's interior we know that it owns a layer of H2 O whose thickness has ... more From the models of Titan's interior we know that it owns a layer of H2 O whose thickness has a value between 550 and 953 km. We solve the heat flux equation considering both radiogenic and accretion heat. We found that the available water in the satellite is distributed in three layers. In surface, a crust of the normal hexagonal
Several distinct regions have been identified by the Voyager encounters within Saturn's magne... more Several distinct regions have been identified by the Voyager encounters within Saturn's magnetosphere. Inside about 400,000 kilometers from Saturn there is a torus of H+ and O+ ions. Strong plasma-wave emissions appear to be associated with the inner torus. At the outer regions of the inner torus some ions have been accelerated to high velocities. In terms of temperature, such
In this work our purpose is to study an acceleration mechanism due the presence of a random elect... more In this work our purpose is to study an acceleration mechanism due the presence of a random electric field. For this calculation we used the measurements of a fluctuating magnetic field obtained by the Voyager 1 and 2 spacecrafts. After that we introduce them into the momentum equation of charged particles seeded in the magnetospheric plasma and -by a Monte
The acceleration of charged particles to suprathermal energies appears to occur in every diffuse ... more The acceleration of charged particles to suprathermal energies appears to occur in every diffuse plasma of astrophysical interest Mechanisms like the direct electrostatic acceleration the stochastic acceleration the diffusive shock acceleration the shock drift acceleration the resonant acceleration by MHD waves the resonant acceleration by Alfven and Langmuir waves the runaway acceleration the acceleration by potential double layers and the
The Voyagers cruises show that in Kronian magnetosphere exists energetic ions and the origin of t... more The Voyagers cruises show that in Kronian magnetosphere exists energetic ions and the origin of their energy is unknown. In this work we propose a mechanism as follows. In the inner magnetosphere of Saturn the corotating plasma produces a velocity shear. We solve the momentum equation; based only on electromagnetic forces, for a charged particle drifted by the corotating plasma
In a previous work we developed a model in which it is possible to estimate the gain and loose of... more In a previous work we developed a model in which it is possible to estimate the gain and loose of energy of a population of ions in the Saturnian's magnetospheric region. Ions like H+, C+, O+, N+, and N2+ are being accelerated to energies of hundreds of MeV. In this work we applied the same model to charged and neutral
In the search of extraterrestrial life it was speculated about the existence of a Circumstellar H... more In the search of extraterrestrial life it was speculated about the existence of a Circumstellar Habitable Zone (CHZ) around stars at which inside planets are suitable for life. Different researches show that the stars types at which CHZ support life are the stars K, G, and F with the type G as the more probable. However in a recent work,
Icarus, 2015
Conditions similar to those observed in the solar wind interaction with Venus and Mars where ther... more Conditions similar to those observed in the solar wind interaction with Venus and Mars where there is a planetary atmosphere in the absence of a global intrinsic magnetic field may also be applicable to Pluto.
section Some of the geomorphological features in Mars are the gullies Some theories developed tri... more section Some of the geomorphological features in Mars are the gullies Some theories developed tried explain its origin either by liquid water liquid carbon dioxide or flows of dry granular material We made a comparative analysis of the Martian gullies with the terrestrial ones We propose that the mechanism of formation of the gullies is as follows In winter CO
Some of the geomorphological features in Mars are the gullies. Some theories developed tried expl... more Some of the geomorphological features in Mars are the gullies. Some theories developed tried explain its origin, either by liquid water, liquid carbon dioxide or flows of dry granular material. We made a comparative analysis of the Martian gullies with the terrestrial ones. We propose that the mechanism of formation of the gullies is as follows: In winter CO2 snow
Theories have been proposed to try to explain the origin of martian gullies, to involve either li... more Theories have been proposed to try to explain the origin of martian gullies, to involve either liquid H2O, liquid CO2 or dry granular material flows. We present a new model of fluidification gases of CO2.
Since their discovery many different theories have been put forward to explain the origin of Mart... more Since their discovery many different theories have been put forward to explain the origin of Martian gullies. Each theory has certain weaknesses, however, and the formation of these features remains poorly understood. Distinctive morphologic variations exist that have often been ignored. Here we present experimental results that attempt to create Martian gullies through gaseous fluidization of CO2 using mixtures of
We estimate the value of Hill s radio for all the extrasolar planets discovered until now It is o... more We estimate the value of Hill s radio for all the extrasolar planets discovered until now It is observed that Hill s radio decrease as the planet decrease it distances to the star Therefore we propose that if the planets had migrated towards it star as proposed by some theories of formation of solar systems then the satellites that the planets could be had was expelled to orbits around it star Then almost all the extrasolar planets near their stars are solitary bodies without satellites We obtain a limit to this condition The expelled satellites could orbit the star in a Trojan position or expelled from the system Only in the case of Earth-likeTrojans we can think that a pre-biotic and biotic chemistry could emerge
In this work we estimate the quantity of planets with life in the Galactic Habitable Zone, using ... more In this work we estimate the quantity of planets with life in the Galactic Habitable Zone, using a modified version of the Drake's equation: [ N_L =sumlimits_i {N_i^* fpi nei fvi } ] where i is the spectral class, NL is the number of planets with life, N*I is the number of stars in the galactic ecosphere of spectral class i, fpi is the fraction of stars that have planets, nei is the number of planets in the circumstellar ecosphere, and fvi is the fraction of planets in the ecosphere with life.
Physics of Plasmas, 1996
An analysis is presented on the motion of contaminant ions picked up by the solar wind within vel... more An analysis is presented on the motion of contaminant ions picked up by the solar wind within velocity shears. An expression is obtained for the ion density in terms of the flow speed across the velocity shear. It is argued that enhanced densities occur in the region where the flow speed is small and that local values may become significantly larger than the ion density outside the velocity shear. A comparison is made with measurements obtained across the plasma wake of comet Giacobini-Zinner with the International Cometary Explorer ͑ICE͒ spacecraft. Within the velocity shear of that comet's ionosheath the cometary ion density becomes large and reaches values that are different from those expected when the ion population depends only on the ionization of a uniform outflow of neutral particles from the cometary nucleus. The enhanced plasma density expected within the velocity shear is compatible with the shape of the density profile of contaminant ions detected in that region.
Journal of Geophysical Research, 2011
1] Measurements conducted with the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-4) instr... more 1] Measurements conducted with the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-4) instrument in the Venus Express spacecraft reveal the presence of a plasma transition within a boundary layer that extends along at the flanks of the Venus ionosheath and where the solar wind exhibits changes similar to those reported from previous missions (Mariner 5, Venera, and Pioneer Venus). At the plasma transition there is a sharp downstream decrease in the density of the solar wind electrons and a sudden increase in their temperature embedded within the boundary layer where more gradual changes in the speed, temperature, and density of the solar wind ions are observed. The ASPERA-4 data also show important fluxes of planetary ions measured downstream from the plasma transition and whose dominant velocity component is in the Sun-Venus direction. The speed of those ions is slower than the local solar wind speed and thus is different from that expected from the convective electric field acceleration in which both speed values should be comparable. The boundary layer is interpreted as representing a feature that results from the transport of solar wind momentum to the Venus upper ionosphere, and the ASPERA-4 data provide information on the kinetic properties of the eroded planetary ion population that is seen to stream mostly in the Sun-Venus direction. From the comparison of the ASPERA-4 measurements with those of the magnetic field obtained with the magnetometer of the Venus Express, it is found that in the near wake crossing of the plasma transition the magnetic field intensity decreases to lower values with downstream distance from the planet in agreement with measurements conducted with the Mariner 5 and the PVO. From the analysis of data for orbits with evidence of the plasma transition within the boundary layer, it is found that the momentum flux of planetary ions measured in the wake can be accounted for from the incident momentum flux of the solar wind protons implying an approximate balance as would result from the transport of solar wind momentum to the planetary particles.
Journal of Geophysical Research, 2009
1] Measurements conducted with the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) instr... more 1] Measurements conducted with the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) instrument of the Mars Express spacecraft provide data of plasma fluxes that stream away from the polar regions of the Mars ionosphere with energy spectra whose peak value increases with distance from the planetary surface. The observed energy distribution reveals a velocity boundary layer with ionospheric plasma that is eroded from the polar regions of the Mars ionosphere and that extends in the downstream direction within a geometry similar to that present along the polar flanks of the Venus ionosheath. The direction of motion of the ionospheric particles in those fluxes is close to that of the solar wind velocity and is not also oriented in a transverse direction as would have been expected if they were solely accelerated by the convective electric field of the solar wind. The ionospheric plasma eroded and deviated by the solar wind within the boundary layer forms a region whose shape is compatible with that of the asymmetric Mars plasma halo that was inferred from the X-ray emission lines measured with the reflecting grating spectrometer of the XMM-Newton telescope. The latter emission is interpreted as resulting from thermal dissipative processes associated with the transport of solar wind momentum to the polar upper ionosphere where both plasma populations interact with each other. Different conditions are applicable throughout most of the dayside hemisphere where the enhanced interplanetary magnetic field intensities that are observed within the ionosphere should make the interaction of the oncoming solar wind plasma with the ionospheric material less efficient. Citation: Pérez-de-Tejada, H., R. Lundin, H. Durand-Manterola, and M. Reyes-Ruiz (2009), Solar wind erosion of the polar regions of the Mars ionosphere,
AIP Conference Proceedings, 2006
From the models of Titan's interior we know that it owns a layer of H2 O whose thickness has ... more From the models of Titan's interior we know that it owns a layer of H2 O whose thickness has a value between 550 and 953 km. We solve the heat flux equation considering both radiogenic and accretion heat. We found that the available water in the satellite is distributed in three layers. In surface, a crust of the normal hexagonal
Several distinct regions have been identified by the Voyager encounters within Saturn's magne... more Several distinct regions have been identified by the Voyager encounters within Saturn's magnetosphere. Inside about 400,000 kilometers from Saturn there is a torus of H+ and O+ ions. Strong plasma-wave emissions appear to be associated with the inner torus. At the outer regions of the inner torus some ions have been accelerated to high velocities. In terms of temperature, such
In this work our purpose is to study an acceleration mechanism due the presence of a random elect... more In this work our purpose is to study an acceleration mechanism due the presence of a random electric field. For this calculation we used the measurements of a fluctuating magnetic field obtained by the Voyager 1 and 2 spacecrafts. After that we introduce them into the momentum equation of charged particles seeded in the magnetospheric plasma and -by a Monte
The acceleration of charged particles to suprathermal energies appears to occur in every diffuse ... more The acceleration of charged particles to suprathermal energies appears to occur in every diffuse plasma of astrophysical interest Mechanisms like the direct electrostatic acceleration the stochastic acceleration the diffusive shock acceleration the shock drift acceleration the resonant acceleration by MHD waves the resonant acceleration by Alfven and Langmuir waves the runaway acceleration the acceleration by potential double layers and the
The Voyagers cruises show that in Kronian magnetosphere exists energetic ions and the origin of t... more The Voyagers cruises show that in Kronian magnetosphere exists energetic ions and the origin of their energy is unknown. In this work we propose a mechanism as follows. In the inner magnetosphere of Saturn the corotating plasma produces a velocity shear. We solve the momentum equation; based only on electromagnetic forces, for a charged particle drifted by the corotating plasma
In a previous work we developed a model in which it is possible to estimate the gain and loose of... more In a previous work we developed a model in which it is possible to estimate the gain and loose of energy of a population of ions in the Saturnian's magnetospheric region. Ions like H+, C+, O+, N+, and N2+ are being accelerated to energies of hundreds of MeV. In this work we applied the same model to charged and neutral
In the search of extraterrestrial life it was speculated about the existence of a Circumstellar H... more In the search of extraterrestrial life it was speculated about the existence of a Circumstellar Habitable Zone (CHZ) around stars at which inside planets are suitable for life. Different researches show that the stars types at which CHZ support life are the stars K, G, and F with the type G as the more probable. However in a recent work,
Icarus, 2015
Conditions similar to those observed in the solar wind interaction with Venus and Mars where ther... more Conditions similar to those observed in the solar wind interaction with Venus and Mars where there is a planetary atmosphere in the absence of a global intrinsic magnetic field may also be applicable to Pluto.
section Some of the geomorphological features in Mars are the gullies Some theories developed tri... more section Some of the geomorphological features in Mars are the gullies Some theories developed tried explain its origin either by liquid water liquid carbon dioxide or flows of dry granular material We made a comparative analysis of the Martian gullies with the terrestrial ones We propose that the mechanism of formation of the gullies is as follows In winter CO
Some of the geomorphological features in Mars are the gullies. Some theories developed tried expl... more Some of the geomorphological features in Mars are the gullies. Some theories developed tried explain its origin, either by liquid water, liquid carbon dioxide or flows of dry granular material. We made a comparative analysis of the Martian gullies with the terrestrial ones. We propose that the mechanism of formation of the gullies is as follows: In winter CO2 snow
Theories have been proposed to try to explain the origin of martian gullies, to involve either li... more Theories have been proposed to try to explain the origin of martian gullies, to involve either liquid H2O, liquid CO2 or dry granular material flows. We present a new model of fluidification gases of CO2.
Since their discovery many different theories have been put forward to explain the origin of Mart... more Since their discovery many different theories have been put forward to explain the origin of Martian gullies. Each theory has certain weaknesses, however, and the formation of these features remains poorly understood. Distinctive morphologic variations exist that have often been ignored. Here we present experimental results that attempt to create Martian gullies through gaseous fluidization of CO2 using mixtures of
We estimate the value of Hill s radio for all the extrasolar planets discovered until now It is o... more We estimate the value of Hill s radio for all the extrasolar planets discovered until now It is observed that Hill s radio decrease as the planet decrease it distances to the star Therefore we propose that if the planets had migrated towards it star as proposed by some theories of formation of solar systems then the satellites that the planets could be had was expelled to orbits around it star Then almost all the extrasolar planets near their stars are solitary bodies without satellites We obtain a limit to this condition The expelled satellites could orbit the star in a Trojan position or expelled from the system Only in the case of Earth-likeTrojans we can think that a pre-biotic and biotic chemistry could emerge
In this work we estimate the quantity of planets with life in the Galactic Habitable Zone, using ... more In this work we estimate the quantity of planets with life in the Galactic Habitable Zone, using a modified version of the Drake's equation: [ N_L =sumlimits_i {N_i^* fpi nei fvi } ] where i is the spectral class, NL is the number of planets with life, N*I is the number of stars in the galactic ecosphere of spectral class i, fpi is the fraction of stars that have planets, nei is the number of planets in the circumstellar ecosphere, and fvi is the fraction of planets in the ecosphere with life.
Physics of Plasmas, 1996
An analysis is presented on the motion of contaminant ions picked up by the solar wind within vel... more An analysis is presented on the motion of contaminant ions picked up by the solar wind within velocity shears. An expression is obtained for the ion density in terms of the flow speed across the velocity shear. It is argued that enhanced densities occur in the region where the flow speed is small and that local values may become significantly larger than the ion density outside the velocity shear. A comparison is made with measurements obtained across the plasma wake of comet Giacobini-Zinner with the International Cometary Explorer ͑ICE͒ spacecraft. Within the velocity shear of that comet's ionosheath the cometary ion density becomes large and reaches values that are different from those expected when the ion population depends only on the ionization of a uniform outflow of neutral particles from the cometary nucleus. The enhanced plasma density expected within the velocity shear is compatible with the shape of the density profile of contaminant ions detected in that region.
Journal of Geophysical Research, 2011
1] Measurements conducted with the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-4) instr... more 1] Measurements conducted with the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-4) instrument in the Venus Express spacecraft reveal the presence of a plasma transition within a boundary layer that extends along at the flanks of the Venus ionosheath and where the solar wind exhibits changes similar to those reported from previous missions (Mariner 5, Venera, and Pioneer Venus). At the plasma transition there is a sharp downstream decrease in the density of the solar wind electrons and a sudden increase in their temperature embedded within the boundary layer where more gradual changes in the speed, temperature, and density of the solar wind ions are observed. The ASPERA-4 data also show important fluxes of planetary ions measured downstream from the plasma transition and whose dominant velocity component is in the Sun-Venus direction. The speed of those ions is slower than the local solar wind speed and thus is different from that expected from the convective electric field acceleration in which both speed values should be comparable. The boundary layer is interpreted as representing a feature that results from the transport of solar wind momentum to the Venus upper ionosphere, and the ASPERA-4 data provide information on the kinetic properties of the eroded planetary ion population that is seen to stream mostly in the Sun-Venus direction. From the comparison of the ASPERA-4 measurements with those of the magnetic field obtained with the magnetometer of the Venus Express, it is found that in the near wake crossing of the plasma transition the magnetic field intensity decreases to lower values with downstream distance from the planet in agreement with measurements conducted with the Mariner 5 and the PVO. From the analysis of data for orbits with evidence of the plasma transition within the boundary layer, it is found that the momentum flux of planetary ions measured in the wake can be accounted for from the incident momentum flux of the solar wind protons implying an approximate balance as would result from the transport of solar wind momentum to the planetary particles.
Journal of Geophysical Research, 2009
1] Measurements conducted with the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) instr... more 1] Measurements conducted with the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) instrument of the Mars Express spacecraft provide data of plasma fluxes that stream away from the polar regions of the Mars ionosphere with energy spectra whose peak value increases with distance from the planetary surface. The observed energy distribution reveals a velocity boundary layer with ionospheric plasma that is eroded from the polar regions of the Mars ionosphere and that extends in the downstream direction within a geometry similar to that present along the polar flanks of the Venus ionosheath. The direction of motion of the ionospheric particles in those fluxes is close to that of the solar wind velocity and is not also oriented in a transverse direction as would have been expected if they were solely accelerated by the convective electric field of the solar wind. The ionospheric plasma eroded and deviated by the solar wind within the boundary layer forms a region whose shape is compatible with that of the asymmetric Mars plasma halo that was inferred from the X-ray emission lines measured with the reflecting grating spectrometer of the XMM-Newton telescope. The latter emission is interpreted as resulting from thermal dissipative processes associated with the transport of solar wind momentum to the polar upper ionosphere where both plasma populations interact with each other. Different conditions are applicable throughout most of the dayside hemisphere where the enhanced interplanetary magnetic field intensities that are observed within the ionosphere should make the interaction of the oncoming solar wind plasma with the ionospheric material less efficient. Citation: Pérez-de-Tejada, H., R. Lundin, H. Durand-Manterola, and M. Reyes-Ruiz (2009), Solar wind erosion of the polar regions of the Mars ionosphere,