Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models

We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations pro...
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Autor*in:	Curry, S. M [verfasserIn] Luhmann, J. G Ma, Y. J Dong, C. F Brain, D Leblanc, F Modolo, R Dong, Y McFadden, J Halekas, J Connerney, J Espley, J Hara, T Harada, Y Lee, C Fang, X Jakosky, B

Format:	Artikel
Sprache:	Englisch

Erschienen:	2015

Rechteinformationen:	Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved.

Schlagwörter:	pickup ions Mars ICME escape precipitation Ions Solar flares Solar physics

Übergeordnetes Werk:	Enthalten in: Geophysical research letters - Washington, DC : Union, 1974, 42(2015), 21, Seite 9095-9102
Übergeordnetes Werk:	volume:42 ; year:2015 ; number:21 ; pages:9095-9102

Links:	Volltext Link aufrufen Link aufrufen

DOI / URN:	10.1002/2015GL065304

Katalog-ID:	OLC1964143268

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520			\|a We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. The shock phase of an ICME drives the most ion escape at Mars The shock phase of an ICME has an O + escape rate of 4.1e25/s O sputtering from the shock phase of an ICME may be on the order of 1e26/s
540			\|a Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved.
650		4	\|a pickup ions
650		4	\|a Mars
650		4	\|a ICME
650		4	\|a escape
650		4	\|a precipitation
650		4	\|a Ions
650		4	\|a Solar flares
650		4	\|a Solar physics
700	1		\|a Luhmann, J. G \|4 oth
700	1		\|a Ma, Y. J \|4 oth
700	1		\|a Dong, C. F \|4 oth
700	1		\|a Brain, D \|4 oth
700	1		\|a Leblanc, F \|4 oth
700	1		\|a Modolo, R \|4 oth
700	1		\|a Dong, Y \|4 oth
700	1		\|a McFadden, J \|4 oth
700	1		\|a Halekas, J \|4 oth
700	1		\|a Connerney, J \|4 oth
700	1		\|a Espley, J \|4 oth
700	1		\|a Hara, T \|4 oth
700	1		\|a Harada, Y \|4 oth
700	1		\|a Lee, C \|4 oth
700	1		\|a Fang, X \|4 oth
700	1		\|a Jakosky, B \|4 oth
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856	4	1	\|u http://dx.doi.org/10.1002/2015GL065304 \|3 Volltext
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allfields	10.1002/2015GL065304 doi PQ20160617 (DE-627)OLC1964143268 (DE-599)GBVOLC1964143268 (PRQ)p952-1f914d63e423ba0efa8a4073e0f877f9561d4f336c398876aae1f0ff58c17a6e0 (KEY)0026932820150000042002109095responseofmarsopickupionstothe8march2015icmeinfere DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Curry, S. M verfasserin aut Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. The shock phase of an ICME drives the most ion escape at Mars The shock phase of an ICME has an O + escape rate of 4.1e25/s O sputtering from the shock phase of an ICME may be on the order of 1e26/s Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. pickup ions Mars ICME escape precipitation Ions Solar flares Solar physics Luhmann, J. G oth Ma, Y. J oth Dong, C. F oth Brain, D oth Leblanc, F oth Modolo, R oth Dong, Y oth McFadden, J oth Halekas, J oth Connerney, J oth Espley, J oth Hara, T oth Harada, Y oth Lee, C oth Fang, X oth Jakosky, B oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9095-9102 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9095-9102 http://dx.doi.org/10.1002/2015GL065304 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL065304/abstract http://search.proquest.com/docview/1756229496 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9095-9102
spelling	10.1002/2015GL065304 doi PQ20160617 (DE-627)OLC1964143268 (DE-599)GBVOLC1964143268 (PRQ)p952-1f914d63e423ba0efa8a4073e0f877f9561d4f336c398876aae1f0ff58c17a6e0 (KEY)0026932820150000042002109095responseofmarsopickupionstothe8march2015icmeinfere DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Curry, S. M verfasserin aut Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. The shock phase of an ICME drives the most ion escape at Mars The shock phase of an ICME has an O + escape rate of 4.1e25/s O sputtering from the shock phase of an ICME may be on the order of 1e26/s Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. pickup ions Mars ICME escape precipitation Ions Solar flares Solar physics Luhmann, J. G oth Ma, Y. J oth Dong, C. F oth Brain, D oth Leblanc, F oth Modolo, R oth Dong, Y oth McFadden, J oth Halekas, J oth Connerney, J oth Espley, J oth Hara, T oth Harada, Y oth Lee, C oth Fang, X oth Jakosky, B oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9095-9102 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9095-9102 http://dx.doi.org/10.1002/2015GL065304 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL065304/abstract http://search.proquest.com/docview/1756229496 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9095-9102
allfields_unstemmed	10.1002/2015GL065304 doi PQ20160617 (DE-627)OLC1964143268 (DE-599)GBVOLC1964143268 (PRQ)p952-1f914d63e423ba0efa8a4073e0f877f9561d4f336c398876aae1f0ff58c17a6e0 (KEY)0026932820150000042002109095responseofmarsopickupionstothe8march2015icmeinfere DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Curry, S. M verfasserin aut Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. The shock phase of an ICME drives the most ion escape at Mars The shock phase of an ICME has an O + escape rate of 4.1e25/s O sputtering from the shock phase of an ICME may be on the order of 1e26/s Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. pickup ions Mars ICME escape precipitation Ions Solar flares Solar physics Luhmann, J. G oth Ma, Y. J oth Dong, C. F oth Brain, D oth Leblanc, F oth Modolo, R oth Dong, Y oth McFadden, J oth Halekas, J oth Connerney, J oth Espley, J oth Hara, T oth Harada, Y oth Lee, C oth Fang, X oth Jakosky, B oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9095-9102 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9095-9102 http://dx.doi.org/10.1002/2015GL065304 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL065304/abstract http://search.proquest.com/docview/1756229496 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9095-9102
allfieldsGer	10.1002/2015GL065304 doi PQ20160617 (DE-627)OLC1964143268 (DE-599)GBVOLC1964143268 (PRQ)p952-1f914d63e423ba0efa8a4073e0f877f9561d4f336c398876aae1f0ff58c17a6e0 (KEY)0026932820150000042002109095responseofmarsopickupionstothe8march2015icmeinfere DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Curry, S. M verfasserin aut Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. The shock phase of an ICME drives the most ion escape at Mars The shock phase of an ICME has an O + escape rate of 4.1e25/s O sputtering from the shock phase of an ICME may be on the order of 1e26/s Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. pickup ions Mars ICME escape precipitation Ions Solar flares Solar physics Luhmann, J. G oth Ma, Y. J oth Dong, C. F oth Brain, D oth Leblanc, F oth Modolo, R oth Dong, Y oth McFadden, J oth Halekas, J oth Connerney, J oth Espley, J oth Hara, T oth Harada, Y oth Lee, C oth Fang, X oth Jakosky, B oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9095-9102 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9095-9102 http://dx.doi.org/10.1002/2015GL065304 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL065304/abstract http://search.proquest.com/docview/1756229496 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9095-9102
allfieldsSound	10.1002/2015GL065304 doi PQ20160617 (DE-627)OLC1964143268 (DE-599)GBVOLC1964143268 (PRQ)p952-1f914d63e423ba0efa8a4073e0f877f9561d4f336c398876aae1f0ff58c17a6e0 (KEY)0026932820150000042002109095responseofmarsopickupionstothe8march2015icmeinfere DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Curry, S. M verfasserin aut Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. The shock phase of an ICME drives the most ion escape at Mars The shock phase of an ICME has an O + escape rate of 4.1e25/s O sputtering from the shock phase of an ICME may be on the order of 1e26/s Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. pickup ions Mars ICME escape precipitation Ions Solar flares Solar physics Luhmann, J. G oth Ma, Y. J oth Dong, C. F oth Brain, D oth Leblanc, F oth Modolo, R oth Dong, Y oth McFadden, J oth Halekas, J oth Connerney, J oth Espley, J oth Hara, T oth Harada, Y oth Lee, C oth Fang, X oth Jakosky, B oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9095-9102 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9095-9102 http://dx.doi.org/10.1002/2015GL065304 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL065304/abstract http://search.proquest.com/docview/1756229496 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9095-9102
language	English
source	Enthalten in Geophysical research letters 42(2015), 21, Seite 9095-9102 volume:42 year:2015 number:21 pages:9095-9102
sourceStr	Enthalten in Geophysical research letters 42(2015), 21, Seite 9095-9102 volume:42 year:2015 number:21 pages:9095-9102
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	pickup ions Mars ICME escape precipitation Ions Solar flares Solar physics
dewey-raw	550
isfreeaccess_bool	false
container_title	Geophysical research letters
authorswithroles_txt_mv	Curry, S. M @@aut@@ Luhmann, J. G @@oth@@ Ma, Y. J @@oth@@ Dong, C. F @@oth@@ Brain, D @@oth@@ Leblanc, F @@oth@@ Modolo, R @@oth@@ Dong, Y @@oth@@ McFadden, J @@oth@@ Halekas, J @@oth@@ Connerney, J @@oth@@ Espley, J @@oth@@ Hara, T @@oth@@ Harada, Y @@oth@@ Lee, C @@oth@@ Fang, X @@oth@@ Jakosky, B @@oth@@
publishDateDaySort_date	2015-01-01T00:00:00Z
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M</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2015</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">ohne Hilfsmittel zu benutzen</subfield><subfield code="b">n</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Band</subfield><subfield code="b">nc</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. 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author	Curry, S. M
spellingShingle	Curry, S. M ddc 550 bkl 38.70 misc pickup ions misc Mars misc ICME misc escape misc precipitation misc Ions misc Solar flares misc Solar physics Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models
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topic_title	550 DNB 38.70 bkl Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models pickup ions Mars ICME escape precipitation Ions Solar flares Solar physics
topic	ddc 550 bkl 38.70 misc pickup ions misc Mars misc ICME misc escape misc precipitation misc Ions misc Solar flares misc Solar physics
topic_unstemmed	ddc 550 bkl 38.70 misc pickup ions misc Mars misc ICME misc escape misc precipitation misc Ions misc Solar flares misc Solar physics
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title	Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models
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title_full	Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models
author_sort	Curry, S. M
journal	Geophysical research letters
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author-letter	Curry, S. M
doi_str_mv	10.1002/2015GL065304
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title_sort	response of mars o+ pickup ions to the 8 march 2015 icme: inferences from maven data‐based models
title_auth	Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models
abstract	We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. The shock phase of an ICME drives the most ion escape at Mars The shock phase of an ICME has an O + escape rate of 4.1e25/s O sputtering from the shock phase of an ICME may be on the order of 1e26/s
abstractGer	We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. The shock phase of an ICME drives the most ion escape at Mars The shock phase of an ICME has an O + escape rate of 4.1e25/s O sputtering from the shock phase of an ICME may be on the order of 1e26/s
abstract_unstemmed	We simulate and compare three phases of the Mars‐solar wind interaction with the 8 March interplanetary coronal mass ejection (ICME) event using Mars Atmosphere and Volatile EvolutioN (MAVEN) mission observations in order to derive heavy ion precipitation and escape rates. The MAVEN observations provide the initial conditions for three steady state MHD model cases, which reproduce the observed features in the solar wind density, velocity, and magnetic field seen along the MAVEN orbit. Applying the MHD results to a kinetic test particle model, we simulate global precipitation and escape maps of O + during the (1) pre‐ICME phase, (2) sheath phase, and (3) ejecta phase. We find that the Case 1 had the lowest precipitation and escape rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , Case 2 had the highest rates of 9.5 × 10 25 and 4.1 × 10 25 s −1 , and Case 3 had rates of 3.2 × 10 25 and 1.3 × 10 25 s −1 , respectively. Additionally, Case 2 produced a high‐energy escaping plume >10 keV, which mirrored corresponding STATIC observations. The shock phase of an ICME drives the most ion escape at Mars The shock phase of an ICME has an O + escape rate of 4.1e25/s O sputtering from the shock phase of an ICME may be on the order of 1e26/s
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container_issue	21
title_short	Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data‐based models
url	http://dx.doi.org/10.1002/2015GL065304 http://onlinelibrary.wiley.com/doi/10.1002/2015GL065304/abstract http://search.proquest.com/docview/1756229496
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author2	Luhmann, J. G Ma, Y. J Dong, C. F Brain, D Leblanc, F Modolo, R Dong, Y McFadden, J Halekas, J Connerney, J Espley, J Hara, T Harada, Y Lee, C Fang, X Jakosky, B
author2Str	Luhmann, J. G Ma, Y. J Dong, C. F Brain, D Leblanc, F Modolo, R Dong, Y McFadden, J Halekas, J Connerney, J Espley, J Hara, T Harada, Y Lee, C Fang, X Jakosky, B
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doi_str	10.1002/2015GL065304
up_date	2024-07-04T07:16:41.502Z
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