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4 results on '"McKenna-Lawler, S."'

1. Plasma Acceleration above Martian Magnetic Anomalies

Author

Lundin, R., Winningham, D., Barabash, S., Frahm, R., Holmström, M., Sauvaud, J. A., Fedorov, A., Asamura, K., Coates, A. J., Soobiah, Y., Hsieh, K. C., Grande, M., Koskinen, H., Kallio, E., Kozyra, J., Woch, J., Fraenz, M., Brain, D., Luhmann, J., McKenna-Lawler, S., Orsini, R. S., Brandt, P., and Wurz, P.

Published
2006

2. Solar Wind-Induced Atmospheric Erosion at Mars: First Results from ASPERA-3 on Mars Express

Author

Lundin, R., Barabash, S., Andersson, H., Holmström, M., Grigoriev, A., Yamauchi, M., Fedorov, A., Budnik, E., Winningham, D., Frahm, R., Scherrer, J., Sharber, J., Asamura, K., Hayakawa, H., Coates, A., Linder, D. R., Curtis, C., Hsieh, K. C., Sandel, B. R., Grande, M., Carter, M., Reading, D. H., Koskinen, H., Kallio, E., Riihela, P., Schmidt, W., Säles, T., Kozyra, J., Krupp, N., Woch, J., Luhmann, J., McKenna-Lawler, S., Cerulli-Irelli, R., Orsini, S., Maggi, M., Mura, A., Milillo, A., Roelof, E., Williams, D., Livi, S., Brandt, P., Wurz, P., and Bochsler, P.

Published
2004

3. Plasma Acceleration Above Martian Magnetic Anomalies

Author

Lundin, R., Winningham, D., Barabash, S., Frahm, R., Holmstrom, M., Sauvaud, J.-A., Fedorov, A., Asamura, Kazushi, Coates, A. J., Soobiah, Y., Hsieh, K. C., Grande, M., Koskinen, H., Kallio, E., Kozyra, J., Woch, J., Fraenz, M., Brain, D., Luhmann, J., McKenna-Lawler, S., Orsini, R. S., Brandt, P., Wurz, P., 浅村, 和史, Lundin, R., Winningham, D., Barabash, S., Frahm, R., Holmstrom, M., Sauvaud, J.-A., Fedorov, A., Asamura, Kazushi, Coates, A. J., Soobiah, Y., Hsieh, K. C., Grande, M., Koskinen, H., Kallio, E., Kozyra, J., Woch, J., Fraenz, M., Brain, D., Luhmann, J., McKenna-Lawler, S., Orsini, R. S., Brandt, P., Wurz, P., and 浅村, 和史

Abstract

著者人数: 23名, Accepted: 2006-01-05

Published
2018

4. Mass composition of the escaping plasma at Mars

Author

Carlsson, Ella, Fedorov, A., Barabash, S., Budnik, E., Grigoriev, A., Gunell, H., Nilsson, H., Sauvaud, J.-A., Lundin, R., Futaana, Y., Holmström, M., Andersson, H., Yamauchi, M., Winningham, J.D., Frahm, R.A., Sharber, J.R., Scherrer, J., Coates, A.J., Linder, D.R., Kataria, D.O., Kallio, E., Koskinen, H., Säles, T., Riihelä, P., Schmidt, W., Kozyra, J., Luhmann, J., Roelof, E., Williams, D., Livi, S., Curtis, C.C., Hsieh, K.C., Sandel, B.R., Grande, M., Carter, M., Thocaven, J.-J., McKenna-Lawler, S., Orsini, S., Cerulli-Irelli, R., Maggi, M., Wurz, P., Bochsler, P., Krupp, N., Woch, J., Fränz, M., Asamura, K., Dierker, C., Carlsson, Ella, Fedorov, A., Barabash, S., Budnik, E., Grigoriev, A., Gunell, H., Nilsson, H., Sauvaud, J.-A., Lundin, R., Futaana, Y., Holmström, M., Andersson, H., Yamauchi, M., Winningham, J.D., Frahm, R.A., Sharber, J.R., Scherrer, J., Coates, A.J., Linder, D.R., Kataria, D.O., Kallio, E., Koskinen, H., Säles, T., Riihelä, P., Schmidt, W., Kozyra, J., Luhmann, J., Roelof, E., Williams, D., Livi, S., Curtis, C.C., Hsieh, K.C., Sandel, B.R., Grande, M., Carter, M., Thocaven, J.-J., McKenna-Lawler, S., Orsini, S., Cerulli-Irelli, R., Maggi, M., Wurz, P., Bochsler, P., Krupp, N., Woch, J., Fränz, M., Asamura, K., and Dierker, C.

Abstract

Data from the Ion Mass Analyzer (IMA) sensor of the ASPERA-3 instrument suite on Mars Express have been analyzed to determine the mass composition of the escaping ion species at Mars. We have examined 77 different ion-beam events and we present the results in terms of flux ratios between the following ion species: CO2+/O+ and O-2(+)/O+. The following ratios averaged over all events and energies were identified: CO2+/O+ = 0.2 and O-2(+)/O+ = 0.9. The values measured are significantly higher, by a factor of 10 for O-2(+)/O+, than a contemporary modeled ratio for the maximum fluxes which the martian ionosphere can supply. The most abundant ion species was found to be O+, followed by O-2(+) and CO2+. We estimate the loss of CO2+ to be 4.0 x 10(24) s(-1) (0.29 kg s(-1)) by using the previous measurements of Phobos-2 in our calculations. The dependence of the ion ratios in relation to their energy ranges we studied, 0.3-3.0 keV, indicated that no clear correlation was found., Validerad; 2006; Bibliografisk uppgift: Se artikeln för de andra 46 medförfattarna.; 20070104 (pafi)

Published
2006
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