Comparison of Martian surface ionizing radiation measurements from MSL-RAD with Badhwar-O'Neill 2011/HZETRN model calculations

Myung-Hee Y. Kim; Francis A. Cucinotta; Hatem N. Nounu; Cary Zeitlin; Donald M. Hassler; Scot C.R. Rafkin; Robert F. Wimmer-Schweingruber; Bent Ehresmann; David E. Brinza; Stephan Böttcher; Eckart Böhm; Soenke Burmeister; Jingnan Guo; Jan Koehler; Cesar Martin; Guenther Reitz; Arik Posner; Javier Gómez-Elvira; Ari-Matti Harri; MSL Science Team

doi:10.1002/2013JE004549

Comparison of Martian surface ionizing radiation measurements from MSL-RAD with Badhwar-O'Neill 2011/HZETRN model calculations

Myung-Hee Y. Kim^*, Francis A. Cucinotta, Hatem N. Nounu, Cary Zeitlin, Donald M. Hassler, Scot C.R. Rafkin, Robert F. Wimmer-Schweingruber, Bent Ehresmann, David E. Brinza, Stephan Böttcher, Eckart Böhm, Soenke Burmeister, Jingnan Guo, Jan Koehler, Cesar Martin, Guenther Reitz, Arik Posner, Javier Gómez-Elvira, Ari-Matti Harri, MSL Science Team

^*Corresponding author for this work

Geology and Geophysics

Research output: Contribution to journal › Article › peer-review

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Abstract

Dose rate measurements from Mars Science Laboratory-radiation assessment detector (MSL-RAD) for 300 sols on Mars are compared to simulation results using the Badhwar-O'Neill 2011 galactic cosmic ray (GCR) environment model and the high-charge and energy transport (HZETRN) code. For the nuclear interactions of primary GCR through Mars atmosphere and Curiosity rover, the quantum multiple scattering theory of nuclear fragmentation is used. Daily atmospheric pressure is measured at Gale Crater by the MSL Rover Environmental Monitoring Station. Particles impinging on top of the Martian atmosphere reach RAD after traversing varying depths of atmosphere that depend on the slant angles, and the model accounts for shielding of the RAD “E” detector (used for dosimetry) by the rest of the instrument. Simulation of average dose rate is in good agreement with RAD measurements for the first 200 sols and reproduces the observed variation of surface dose rate with changing heliospheric conditions and atmospheric pressure. Model results agree less well between sols 200 and 300 due to subtleties in the changing heliospheric conditions. It also suggests that the average contributions of albedo particles (charge number Z < 3) from Martian regolith comprise about 10% and 42% of the average daily point dose and dose equivalent, respectively. Neutron contributions to tissue-averaged effective doses will be reduced compared to point dose equivalent estimates because a large portion of the neutron point dose is due to low-energy neutrons with energies

Original language	English
Pages (from-to)	1311-1321
Number of pages	11
Journal	Journal of Geophysical Research - Planets
Volume	119
Issue number	6
Early online date	17 Jun 2014
DOIs	https://doi.org/10.1002/2013JE004549
Publication status	Published - Jun 2014

Bibliographical note

RAD is supported by NASA (HEOMD) under Jet Propulsion Laboratory (JPL) subcontract 1273039 to Southwest Research Institute and in Germany by the German Aerospace Center (DLR) and DLR′s Space Administration grant 50QM0501 and 50QM1201 to the Christian‐Albrechts‐Universit at Kiel. Part of this research was carried out at JPL, California Institute of Technology, under a contract with NASA. We thank Jeff Simmonds, John Grotzinger, Joy Crisp, Ashwin Vasvada, and Helen Mortensen at JPL, Gale Allen, Michael Meyer, Chris Moore, Victoria Friedensen at NASA Headquarters, and Heiner Witte at DLR in Germany for their support of RAD. The data used in this paper are archived in the NASA Planetary Data System's Planetary Plasma Interactions Node at the University of California, Los Angeles. The archival volume includes the full binary raw data files, detailed descriptions of the structures therein, and higher‐level data products in human‐readable form. The PPI node is hosted at the following URL: http://ppi.pds.nasa.gov/. We appreciate helpful discussion in BO'11 with Dr. Patrick O'Neill at the NASA Johnson Space Center and in HZETRN with Dr. Francis Badavi at the NASA Langley Research Center.

Keywords

Galactic cosmic radiation
radiation transport
dose rate on Martian surface

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Kim, M.-H. Y., Cucinotta, F. A., Nounu, H. N., Zeitlin, C., Hassler, D. M., Rafkin, S. C. R., Wimmer-Schweingruber, R. F., Ehresmann, B., Brinza, D. E., Böttcher, S., Böhm, E., Burmeister, S., Guo, J., Koehler, J., Martin, C., Reitz, G., Posner, A., Gómez-Elvira, J., Harri, A.-M., & MSL Science Team (2014). Comparison of Martian surface ionizing radiation measurements from MSL-RAD with Badhwar-O'Neill 2011/HZETRN model calculations. Journal of Geophysical Research - Planets, 119(6), 1311-1321. https://doi.org/10.1002/2013JE004549

Kim, M-HY, Cucinotta, FA, Nounu, HN, Zeitlin, C, Hassler, DM, Rafkin, SCR, Wimmer-Schweingruber, RF, Ehresmann, B, Brinza, DE, Böttcher, S, Böhm, E, Burmeister, S, Guo, J, Koehler, J, Martin, C, Reitz, G, Posner, A, Gómez-Elvira, J, Harri, A-M & MSL Science Team 2014, 'Comparison of Martian surface ionizing radiation measurements from MSL-RAD with Badhwar-O'Neill 2011/HZETRN model calculations', Journal of Geophysical Research - Planets, vol. 119, no. 6, pp. 1311-1321. https://doi.org/10.1002/2013JE004549

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title = "Comparison of Martian surface ionizing radiation measurements from MSL-RAD with Badhwar-O'Neill 2011/HZETRN model calculations",

abstract = "Dose rate measurements from Mars Science Laboratory-radiation assessment detector (MSL-RAD) for 300 sols on Mars are compared to simulation results using the Badhwar-O'Neill 2011 galactic cosmic ray (GCR) environment model and the high-charge and energy transport (HZETRN) code. For the nuclear interactions of primary GCR through Mars atmosphere and Curiosity rover, the quantum multiple scattering theory of nuclear fragmentation is used. Daily atmospheric pressure is measured at Gale Crater by the MSL Rover Environmental Monitoring Station. Particles impinging on top of the Martian atmosphere reach RAD after traversing varying depths of atmosphere that depend on the slant angles, and the model accounts for shielding of the RAD “E” detector (used for dosimetry) by the rest of the instrument. Simulation of average dose rate is in good agreement with RAD measurements for the first 200 sols and reproduces the observed variation of surface dose rate with changing heliospheric conditions and atmospheric pressure. Model results agree less well between sols 200 and 300 due to subtleties in the changing heliospheric conditions. It also suggests that the average contributions of albedo particles (charge number Z < 3) from Martian regolith comprise about 10% and 42% of the average daily point dose and dose equivalent, respectively. Neutron contributions to tissue-averaged effective doses will be reduced compared to point dose equivalent estimates because a large portion of the neutron point dose is due to low-energy neutrons with energies ",

keywords = "Galactic cosmic radiation, radiation transport, dose rate on Martian surface",

author = "Kim, {Myung-Hee Y.} and Cucinotta, {Francis A.} and Nounu, {Hatem N.} and Cary Zeitlin and Hassler, {Donald M.} and Rafkin, {Scot C.R.} and Wimmer-Schweingruber, {Robert F.} and Bent Ehresmann and Brinza, {David E.} and Stephan B{\"o}ttcher and Eckart B{\"o}hm and Soenke Burmeister and Jingnan Guo and Jan Koehler and Cesar Martin and Guenther Reitz and Arik Posner and Javier G{\'o}mez-Elvira and Ari-Matti Harri and {MSL Science Team} and Javier Martin-Torres",

note = "RAD is supported by NASA (HEOMD) under Jet Propulsion Laboratory (JPL) subcontract 1273039 to Southwest Research Institute and in Germany by the German Aerospace Center (DLR) and DLR′s Space Administration grant 50QM0501 and 50QM1201 to the Christian‐Albrechts‐Universit at Kiel. Part of this research was carried out at JPL, California Institute of Technology, under a contract with NASA. We thank Jeff Simmonds, John Grotzinger, Joy Crisp, Ashwin Vasvada, and Helen Mortensen at JPL, Gale Allen, Michael Meyer, Chris Moore, Victoria Friedensen at NASA Headquarters, and Heiner Witte at DLR in Germany for their support of RAD. The data used in this paper are archived in the NASA Planetary Data System's Planetary Plasma Interactions Node at the University of California, Los Angeles. The archival volume includes the full binary raw data files, detailed descriptions of the structures therein, and higher‐level data products in human‐readable form. The PPI node is hosted at the following URL: http://ppi.pds.nasa.gov/. We appreciate helpful discussion in BO'11 with Dr. Patrick O'Neill at the NASA Johnson Space Center and in HZETRN with Dr. Francis Badavi at the NASA Langley Research Center.",

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AU - Kim, Myung-Hee Y.

AU - Cucinotta, Francis A.

AU - Nounu, Hatem N.

AU - Zeitlin, Cary

AU - Hassler, Donald M.

AU - Rafkin, Scot C.R.

AU - Wimmer-Schweingruber, Robert F.

AU - Ehresmann, Bent

AU - Brinza, David E.

AU - Böttcher, Stephan

AU - Böhm, Eckart

AU - Burmeister, Soenke

AU - Guo, Jingnan

AU - Koehler, Jan

AU - Martin, Cesar

AU - Reitz, Guenther

AU - Posner, Arik

AU - Gómez-Elvira, Javier

AU - Harri, Ari-Matti

AU - MSL Science Team

AU - Martin-Torres, Javier

N1 - RAD is supported by NASA (HEOMD) under Jet Propulsion Laboratory (JPL) subcontract 1273039 to Southwest Research Institute and in Germany by the German Aerospace Center (DLR) and DLR′s Space Administration grant 50QM0501 and 50QM1201 to the Christian‐Albrechts‐Universit at Kiel. Part of this research was carried out at JPL, California Institute of Technology, under a contract with NASA. We thank Jeff Simmonds, John Grotzinger, Joy Crisp, Ashwin Vasvada, and Helen Mortensen at JPL, Gale Allen, Michael Meyer, Chris Moore, Victoria Friedensen at NASA Headquarters, and Heiner Witte at DLR in Germany for their support of RAD. The data used in this paper are archived in the NASA Planetary Data System's Planetary Plasma Interactions Node at the University of California, Los Angeles. The archival volume includes the full binary raw data files, detailed descriptions of the structures therein, and higher‐level data products in human‐readable form. The PPI node is hosted at the following URL: http://ppi.pds.nasa.gov/. We appreciate helpful discussion in BO'11 with Dr. Patrick O'Neill at the NASA Johnson Space Center and in HZETRN with Dr. Francis Badavi at the NASA Langley Research Center.

PY - 2014/6

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N2 - Dose rate measurements from Mars Science Laboratory-radiation assessment detector (MSL-RAD) for 300 sols on Mars are compared to simulation results using the Badhwar-O'Neill 2011 galactic cosmic ray (GCR) environment model and the high-charge and energy transport (HZETRN) code. For the nuclear interactions of primary GCR through Mars atmosphere and Curiosity rover, the quantum multiple scattering theory of nuclear fragmentation is used. Daily atmospheric pressure is measured at Gale Crater by the MSL Rover Environmental Monitoring Station. Particles impinging on top of the Martian atmosphere reach RAD after traversing varying depths of atmosphere that depend on the slant angles, and the model accounts for shielding of the RAD “E” detector (used for dosimetry) by the rest of the instrument. Simulation of average dose rate is in good agreement with RAD measurements for the first 200 sols and reproduces the observed variation of surface dose rate with changing heliospheric conditions and atmospheric pressure. Model results agree less well between sols 200 and 300 due to subtleties in the changing heliospheric conditions. It also suggests that the average contributions of albedo particles (charge number Z < 3) from Martian regolith comprise about 10% and 42% of the average daily point dose and dose equivalent, respectively. Neutron contributions to tissue-averaged effective doses will be reduced compared to point dose equivalent estimates because a large portion of the neutron point dose is due to low-energy neutrons with energies

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KW - Galactic cosmic radiation

KW - radiation transport

KW - dose rate on Martian surface

U2 - 10.1002/2013JE004549

DO - 10.1002/2013JE004549

M3 - Article

SN - 2169-9097

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ER -

Comparison of Martian surface ionizing radiation measurements from MSL-RAD with Badhwar-O'Neill 2011/HZETRN model calculations

Abstract

Bibliographical note

Keywords

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