5 results on '"Peter, Kerstin"'
Search Results
2. The effects of atmospheric dust and solar radiation on the dayside ionosphere of Mars derived from 17 years of Mars Express radio science observations
- Author
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Peter, Kerstin, Pätzold, M., Montabone, L., Thiemann, E., González-Galindo, F., Witasse, O., Tellmann, S., Bird, M. K., Ministerio de Ciencia e Innovación (España), and German Research Foundation
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Dust cycle ,Space and Planetary Science ,Radio science ,Mars ,Astronomy and Astrophysics ,Mars Express ,Ionosphere - Abstract
This work combines 17 years of Mars Express radio science (MaRS) observations with proxies for insolation and local/global atmospheric dust to investigate the combined and individual effects on the dayside ionosphere of Mars from the top down to the ionospheric base. The increase in insolation from orbital apocenter to pericenter in combination with Mars‘ dust cycle causes an average rise of the whole photochemically dominated region of the dayside ionosphere, ranging from 13 km at the ionospheric base up to 22 km above the main peak during conditions without a global dust storm. The declining phase of the 2018 global dust storm was observed by MaRS on the southern hemisphere and close to pericenter. The observed lifting effect on the whole photochemically dominated region of the ionosphere from the increased insolation and the high local and global atmospheric dust levels exceeds that seen by MaRS from similar seasons during years without a global dust storm. The average ionospheric peak altitude at the subsolar point rises for increasing levels of local atmospheric dust until a maximum elevation is reached. This maximum depends on the available insolation at the top of the planetary atmosphere. Further increases of the local atmospheric dust levels do not lead to a further rise of the average ionospheric peak altitude in the investigated data set. This indicates a limit for the warming/expansion of the lower neutral atmosphere and the consecutive lifting of the ionosphere based on the available insolation and explains why regional dust storms can cause a similar lifting of the ionospheric main peak region as global dust storms. © 2023 Elsevier Inc. All rights reserved., The Mars Express Radio Science Experiment (MaRS) was funded by BMWi Berlin via the Deutsches Zentrum für Luft- und Raumfahrt (DLR) under the Grant 50QM1802. Support for Mars Express Radio Science at Stanford University was provided by NASA through a JPL Contract. Support for the Multimission Radio Science Support Team was provided by NASA/JPL. Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. We thank everyone involved in the Mars Express project at ESTEC, ESOC, ESAC, JPL, and the ESTRACK and DSN ground stations for their continuous support. K. P., M. P. and S. T. acknowledge funding for this project by the Deutsche Forschungsgemeinschaft (DFG) under Grant PE 3225/2-1, PA 525/25-1 and TE 664/4-1. F.G.G. acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033.
- Published
- 2023
3. The dayside ionospheres of Mars and Venus: Comparing a one-dimensional photochemical model with MaRS (Mars Express) and VeRa (Venus Express) observations.
- Author
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Peter, Kerstin, Pätzold, Martin, Molina-Cuberos, Gregorio, Witasse, Olivier, González-Galindo, F., Withers, Paul, Bird, Michael K., Häusler, Bernd, Hinson, David P., Tellmann, Silvia, and Tyler, G. Leonard
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PLANETARY ionospheres , *VENUS (Planet) , *COMPARATIVE studies , *PHOTOCHEMISTRY , *ASTRONOMICAL observations , *MARS (Planet) - Abstract
Highlights: [•] Development of a flexible 1D photoch. model for the Mars and Venus lower ionospheres. [•] Lower Mars ionosphere behavior (MaRS observations) generally reproduced with the MCD. [•] Best model/MaRS agreement with the MCD low solar flux/clear atmosphere/MY24 scenarios. [•] VenusGRAM (VIRA) is too limited for reproduction of VeRa lower ionosphere observations. [ABSTRACT FROM AUTHOR]
- Published
- 2014
- Full Text
- View/download PDF
4. The lower dayside ionosphere of Mars from 14 years of MaRS radio science observations.
- Author
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Peter, Kerstin, Pätzold, Martin, Molina-Cuberos, Gregorio J., González-Galindo, Francisco, Witasse, Olivier, Tellmann, Silvia, Häusler, Bernd, and Bird, Michael K.
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SOLAR atmosphere , *ELECTRON distribution , *ELECTRON density , *CORONAL mass ejections , *EXCESS electrons , *MARS (Planet) , *IONOSPHERE - Abstract
This work uses a subset of "quiet" MaRS ionospheric dayside observations (MaRS quiet , 2004–2017) and a 1-D photochemical model (IonA-2) to investigate the potential formation processes of the excess electron densities merged with the base of the main ionosphere (Mm). 42% of the investigated MaRS observations contain identified Mm, which occur in a large variety of shapes ranging from smoothly decreasing electron densities to peak structures below the base of M1. The Mm appear over the full range of accessible solar zenith angles (50° - 90°) and are found between approximately 70 and 110 km altitude. Their base is found on average deeper in the atmosphere than the base of the averaged undisturbed MaRS electron density profiles. This indicates a dependence of the Mm formation on energy sources that penetrate deep into the atmosphere. This is supported by a strong positive correlation with increasing solar activity when solar flares, coronal mass ejections, and enhanced short solar X-ray and Ly-α intensities are more common. No relationship is found between the Mm occurrence rate and the magnitude/inclination of the weak crustal crustal magnetic field in MaRS quiet. Investigations with the IonA-2 photochemical model for undisturbed and flare conditions show that the ionization of the local neutral atmosphere by solar X-ray radiation <2 nm provides a satisfying explanation for detected Mm features with smoothly decreasing electron densities below the M1 base in combination with moderate slopes of the lower Mm region α Mm and altitudes of the lower boundary h L , S. While sufficient ionization energy reaches the region of interest during flares, no Mm features with peaks below the M1 base occur in any of the model electron density profiles. This supports the conclusion that the subgroup of merged excess electron densities with peaks or intermediate features (Mi) below the M1 base must have an origin different from the sole variability of solar X-ray radiation during undisturbed and solar flare conditions. The size of the identified Mm makes an exclusive meteoric origin of the Mm peak structures unlikely. It is indicative from the IonA-2 model results that the general increase/decrease of solar X-ray <2 nm leads to a correlated response of the Mm region. The sporadic occurrence of the merged excess electron densities in the MaRS observations is therefore assumed to be a combination of observational (increased observation noise level compared to the available amount of X-ray radiation <2 nm, shift of the lower baseline by ionospheric deviations from radial symmetry) and environmental (e.g. variations in solar X-ray) factors. [ABSTRACT FROM AUTHOR]
- Published
- 2021
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5. Characterization of the lower layer in the dayside Venus ionosphere and comparisons with Mars.
- Author
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Girazian, Zachary, Withers, Paul, Häusler, Bernd, Pätzold, Martin, Tellmann, Silvia, and Peter, Kerstin
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VENUSIAN ionosphere , *MARTIAN ionosphere , *ZENITH distance , *SOLAR radiation , *SOLAR activity - Abstract
The influence of solar zenith angle (SZA) and solar irradiance has been well characterized for the V2 layer in the Venus ionosphere, but not the V1 layer, where previous efforts were limited by data scarcity and incomplete SZA coverage. Here we use more than 200 radio occultation profiles from Venus Express with good SZA coverage to characterize how the V1 peak altitude, peak density, and morphology respond to changes in SZA and solar activity. The V1 and V2 peak altitudes vary little with SZA, and both peak electron densities vary with SZA in an approximately Chapman-like manner. These results imply that the thermal structures of the atmosphere and ionosphere between ∼125 km and ∼140 km vary little with SZA. As solar activity increases, the ratio of the V1 to V2 peak density increases, and the V1 morphology changes more than the V2 morphology. These results are due to the soft X-ray flux increasing relative to the EUV flux as solar activity increases. We compare the behavior of the V1 layer to the analogous M1 layer at Mars, and find that their peak altitudes respond differently to changes in SZA and solar activity. The V1 peak density also increases more with solar activity than the M1 peak density. These distinct behaviors arise from differences in their underlying neutral atmospheres. [ABSTRACT FROM AUTHOR]
- Published
- 2015
- Full Text
- View/download PDF
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