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Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation
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| Zeitschriftentitel: | Journal of Geophysical Research: Space Physics |
|---|---|
| Personen und Körperschaften: | , , , , , |
| In: | Journal of Geophysical Research: Space Physics, 118, 2013, 6, S. 3446-3463 |
| Format: | E-Article |
| Sprache: | Englisch |
| veröffentlicht: |
American Geophysical Union (AGU)
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| author_facet |
Christon, S. P. Hamilton, D. C. DiFabio, R. D. Mitchell, D. G. Krimigis, S. M. Jontof‐Hutter, D. S. Christon, S. P. Hamilton, D. C. DiFabio, R. D. Mitchell, D. G. Krimigis, S. M. Jontof‐Hutter, D. S. |
|---|---|
| author |
Christon, S. P. Hamilton, D. C. DiFabio, R. D. Mitchell, D. G. Krimigis, S. M. Jontof‐Hutter, D. S. |
| spellingShingle |
Christon, S. P. Hamilton, D. C. DiFabio, R. D. Mitchell, D. G. Krimigis, S. M. Jontof‐Hutter, D. S. Journal of Geophysical Research: Space Physics Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation Space and Planetary Science Geophysics |
| author_sort |
christon, s. p. |
| spelling |
Christon, S. P. Hamilton, D. C. DiFabio, R. D. Mitchell, D. G. Krimigis, S. M. Jontof‐Hutter, D. S. 2169-9380 2169-9402 American Geophysical Union (AGU) Space and Planetary Science Geophysics http://dx.doi.org/10.1002/jgra.50383 <jats:p>Suprathermal singly charged molecular ions, O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> (at ~32 Da/e) and the Mass‐28 ion group <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup> (ions at ~28 Da/e, with possible contributions from C<jats:sub>2</jats:sub>H<jats:sub>5</jats:sub><jats:sup>+</jats:sup>, HCNH<jats:sup>+</jats:sup>, N<jats:sub>2</jats:sub><jats:sup>+</jats:sup>, and/or CO<jats:sup>+</jats:sup>), are present throughout Saturn's ~4–20 Rs (1 Saturn radius, Rs = 60,268 km) near‐equatorial magnetosphere from mid‐2004 until mid‐2012. These ~83–167 keV/e heavy ions measured by Cassini's CHarge‐Energy‐Mass Spectrometer have long‐term temporal profiles that differ from each other and differ relative to the dominant water group ions, W<jats:sup>+</jats:sup> (O<jats:sup>+</jats:sup>, OH<jats:sup>+</jats:sup>, H<jats:sub>2</jats:sub>O<jats:sup>+</jats:sup>, and H<jats:sub>3</jats:sub>O<jats:sup>+</jats:sup>). O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup>, initially ~0.05, declined steadily until equinox in mid‐2009 by a factor of ~6, and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup>, initially ~0.007, declined similarly until early‐2007 by a factor of ~2. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> decline is consistent with Cassini's in situ ring‐ionosphere thermal ion measurements, and with proposed and modeled seasonal photolysis of Saturn's rings for thermal O<jats:sub>2</jats:sub> and O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>. The water ice‐dominated main rings and Enceladus plume depositions thereon are the two most likely O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> sources. Enceladus' dynamic plumes, though, have no known long‐term dependence. After declining, O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> levels remained low until late‐2011 when O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> increased, but <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> did not. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> increase was steady and became statistically significant by mid‐2012, indicating a clear increase after a decline, that is, a possibly delayed O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> “seasonal” recovery. Ring insolation is driven by solar UV flux which itself varies with the sun's 11 year activity cycle. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> declines are consistent with seasonal ring insolation. No O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> response to the late‐2008 solar‐cycle UV minimum and recovery is evident. However, the O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> recovery from the postequinox baseline levels in late‐2011 coincided with a strong solar UV enhancement. We suggest a scenario/framework in which the O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> observations can be understood.</jats:p> Saturn suprathermal O<sub>2</sub><sup>+</sup> and mass‐28<sup>+</sup> molecular ions: Long‐term seasonal and solar variation Journal of Geophysical Research: Space Physics |
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10.1002/jgra.50383 |
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Geologie und Paläontologie Geographie Physik Technik |
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American Geophysical Union (AGU), 2013 |
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American Geophysical Union (AGU), 2013 |
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2013 |
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American Geophysical Union (AGU) |
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Journal of Geophysical Research: Space Physics |
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49 |
| title |
Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_unstemmed |
Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_full |
Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_fullStr |
Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_full_unstemmed |
Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_short |
Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_sort |
saturn suprathermal o<sub>2</sub><sup>+</sup> and mass‐28<sup>+</sup> molecular ions: long‐term seasonal and solar variation |
| topic |
Space and Planetary Science Geophysics |
| url |
http://dx.doi.org/10.1002/jgra.50383 |
| publishDate |
2013 |
| physical |
3446-3463 |
| description |
<jats:p>Suprathermal singly charged molecular ions, O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> (at ~32 Da/e) and the Mass‐28 ion group <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup> (ions at ~28 Da/e, with possible contributions from C<jats:sub>2</jats:sub>H<jats:sub>5</jats:sub><jats:sup>+</jats:sup>, HCNH<jats:sup>+</jats:sup>, N<jats:sub>2</jats:sub><jats:sup>+</jats:sup>, and/or CO<jats:sup>+</jats:sup>), are present throughout Saturn's ~4–20 Rs (1 Saturn radius, Rs = 60,268 km) near‐equatorial magnetosphere from mid‐2004 until mid‐2012. These ~83–167 keV/e heavy ions measured by Cassini's CHarge‐Energy‐Mass Spectrometer have long‐term temporal profiles that differ from each other and differ relative to the dominant water group ions, W<jats:sup>+</jats:sup> (O<jats:sup>+</jats:sup>, OH<jats:sup>+</jats:sup>, H<jats:sub>2</jats:sub>O<jats:sup>+</jats:sup>, and H<jats:sub>3</jats:sub>O<jats:sup>+</jats:sup>). O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup>, initially ~0.05, declined steadily until equinox in mid‐2009 by a factor of ~6, and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup>, initially ~0.007, declined similarly until early‐2007 by a factor of ~2. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> decline is consistent with Cassini's in situ ring‐ionosphere thermal ion measurements, and with proposed and modeled seasonal photolysis of Saturn's rings for thermal O<jats:sub>2</jats:sub> and O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>. The water ice‐dominated main rings and Enceladus plume depositions thereon are the two most likely O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> sources. Enceladus' dynamic plumes, though, have no known long‐term dependence. After declining, O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> levels remained low until late‐2011 when O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> increased, but <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> did not. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> increase was steady and became statistically significant by mid‐2012, indicating a clear increase after a decline, that is, a possibly delayed O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> “seasonal” recovery. Ring insolation is driven by solar UV flux which itself varies with the sun's 11 year activity cycle. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> declines are consistent with seasonal ring insolation. No O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> response to the late‐2008 solar‐cycle UV minimum and recovery is evident. However, the O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> recovery from the postequinox baseline levels in late‐2011 coincided with a strong solar UV enhancement. We suggest a scenario/framework in which the O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> observations can be understood.</jats:p> |
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| author | Christon, S. P., Hamilton, D. C., DiFabio, R. D., Mitchell, D. G., Krimigis, S. M., Jontof‐Hutter, D. S. |
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| description | <jats:p>Suprathermal singly charged molecular ions, O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> (at ~32 Da/e) and the Mass‐28 ion group <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup> (ions at ~28 Da/e, with possible contributions from C<jats:sub>2</jats:sub>H<jats:sub>5</jats:sub><jats:sup>+</jats:sup>, HCNH<jats:sup>+</jats:sup>, N<jats:sub>2</jats:sub><jats:sup>+</jats:sup>, and/or CO<jats:sup>+</jats:sup>), are present throughout Saturn's ~4–20 Rs (1 Saturn radius, Rs = 60,268 km) near‐equatorial magnetosphere from mid‐2004 until mid‐2012. These ~83–167 keV/e heavy ions measured by Cassini's CHarge‐Energy‐Mass Spectrometer have long‐term temporal profiles that differ from each other and differ relative to the dominant water group ions, W<jats:sup>+</jats:sup> (O<jats:sup>+</jats:sup>, OH<jats:sup>+</jats:sup>, H<jats:sub>2</jats:sub>O<jats:sup>+</jats:sup>, and H<jats:sub>3</jats:sub>O<jats:sup>+</jats:sup>). O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup>, initially ~0.05, declined steadily until equinox in mid‐2009 by a factor of ~6, and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup>, initially ~0.007, declined similarly until early‐2007 by a factor of ~2. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> decline is consistent with Cassini's in situ ring‐ionosphere thermal ion measurements, and with proposed and modeled seasonal photolysis of Saturn's rings for thermal O<jats:sub>2</jats:sub> and O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>. The water ice‐dominated main rings and Enceladus plume depositions thereon are the two most likely O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> sources. Enceladus' dynamic plumes, though, have no known long‐term dependence. After declining, O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> levels remained low until late‐2011 when O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> increased, but <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> did not. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> increase was steady and became statistically significant by mid‐2012, indicating a clear increase after a decline, that is, a possibly delayed O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> “seasonal” recovery. Ring insolation is driven by solar UV flux which itself varies with the sun's 11 year activity cycle. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> declines are consistent with seasonal ring insolation. No O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> response to the late‐2008 solar‐cycle UV minimum and recovery is evident. However, the O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> recovery from the postequinox baseline levels in late‐2011 coincided with a strong solar UV enhancement. We suggest a scenario/framework in which the O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> observations can be understood.</jats:p> |
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| imprint | American Geophysical Union (AGU), 2013 |
| imprint_str_mv | American Geophysical Union (AGU), 2013 |
| institution | DE-Brt1, DE-Zwi2, DE-D161, DE-Zi4, DE-Gla1, DE-15, DE-Pl11, DE-Rs1, DE-14, DE-105, DE-Ch1, DE-L229, DE-D275, DE-Bn3 |
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| mega_collection | American Geophysical Union (AGU) (CrossRef) |
| physical | 3446-3463 |
| publishDate | 2013 |
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| source_id | 49 |
| spelling | Christon, S. P. Hamilton, D. C. DiFabio, R. D. Mitchell, D. G. Krimigis, S. M. Jontof‐Hutter, D. S. 2169-9380 2169-9402 American Geophysical Union (AGU) Space and Planetary Science Geophysics http://dx.doi.org/10.1002/jgra.50383 <jats:p>Suprathermal singly charged molecular ions, O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> (at ~32 Da/e) and the Mass‐28 ion group <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup> (ions at ~28 Da/e, with possible contributions from C<jats:sub>2</jats:sub>H<jats:sub>5</jats:sub><jats:sup>+</jats:sup>, HCNH<jats:sup>+</jats:sup>, N<jats:sub>2</jats:sub><jats:sup>+</jats:sup>, and/or CO<jats:sup>+</jats:sup>), are present throughout Saturn's ~4–20 Rs (1 Saturn radius, Rs = 60,268 km) near‐equatorial magnetosphere from mid‐2004 until mid‐2012. These ~83–167 keV/e heavy ions measured by Cassini's CHarge‐Energy‐Mass Spectrometer have long‐term temporal profiles that differ from each other and differ relative to the dominant water group ions, W<jats:sup>+</jats:sup> (O<jats:sup>+</jats:sup>, OH<jats:sup>+</jats:sup>, H<jats:sub>2</jats:sub>O<jats:sup>+</jats:sup>, and H<jats:sub>3</jats:sub>O<jats:sup>+</jats:sup>). O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup>, initially ~0.05, declined steadily until equinox in mid‐2009 by a factor of ~6, and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup>, initially ~0.007, declined similarly until early‐2007 by a factor of ~2. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> decline is consistent with Cassini's in situ ring‐ionosphere thermal ion measurements, and with proposed and modeled seasonal photolysis of Saturn's rings for thermal O<jats:sub>2</jats:sub> and O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>. The water ice‐dominated main rings and Enceladus plume depositions thereon are the two most likely O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> sources. Enceladus' dynamic plumes, though, have no known long‐term dependence. After declining, O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> levels remained low until late‐2011 when O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> increased, but <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> did not. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> increase was steady and became statistically significant by mid‐2012, indicating a clear increase after a decline, that is, a possibly delayed O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> “seasonal” recovery. Ring insolation is driven by solar UV flux which itself varies with the sun's 11 year activity cycle. The O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> and <jats:sup>28</jats:sup>M<jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> declines are consistent with seasonal ring insolation. No O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> response to the late‐2008 solar‐cycle UV minimum and recovery is evident. However, the O<jats:sub>2</jats:sub><jats:sup>+</jats:sup>/W<jats:sup>+</jats:sup> recovery from the postequinox baseline levels in late‐2011 coincided with a strong solar UV enhancement. We suggest a scenario/framework in which the O<jats:sub>2</jats:sub><jats:sup>+</jats:sup> observations can be understood.</jats:p> Saturn suprathermal O<sub>2</sub><sup>+</sup> and mass‐28<sup>+</sup> molecular ions: Long‐term seasonal and solar variation Journal of Geophysical Research: Space Physics |
| spellingShingle | Christon, S. P., Hamilton, D. C., DiFabio, R. D., Mitchell, D. G., Krimigis, S. M., Jontof‐Hutter, D. S., Journal of Geophysical Research: Space Physics, Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation, Space and Planetary Science, Geophysics |
| title | Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_full | Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_fullStr | Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_full_unstemmed | Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_short | Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| title_sort | saturn suprathermal o<sub>2</sub><sup>+</sup> and mass‐28<sup>+</sup> molecular ions: long‐term seasonal and solar variation |
| title_unstemmed | Saturn suprathermal O2+ and mass‐28+ molecular ions: Long‐term seasonal and solar variation |
| topic | Space and Planetary Science, Geophysics |
| url | http://dx.doi.org/10.1002/jgra.50383 |