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Climatology and Diurnal Variation of Ozone Column Abundances for 2.5 Mars Years as Measured by the NOMAD‐UVIS Spectrometer.

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Title: Climatology and Diurnal Variation of Ozone Column Abundances for 2.5 Mars Years as Measured by the NOMAD‐UVIS Spectrometer.
Authors: Mason, J. P.1 (AUTHOR) jon.mason@open.ac.uk, Patel, M. R.1,2 (AUTHOR), Holmes, J. A.1 (AUTHOR), Wolff, M. J.3 (AUTHOR), Alday, J.1 (AUTHOR), Streeter, P.1 (AUTHOR), Olsen, K. S.1,4 (AUTHOR), Brown, M. A. J.1,5 (AUTHOR), Sellers, G.1 (AUTHOR), Marriner, C.1 (AUTHOR), Willame, Y.6 (AUTHOR), Thomas, I.6 (AUTHOR), Ristic, B.6 (AUTHOR), Daerden, F.6 (AUTHOR), Vandaele, A. C.6 (AUTHOR), Lopez‐Moreno, J.‐J.7 (AUTHOR), Bellucci, G.8 (AUTHOR)
Source: Journal of Geophysical Research. Planets. Apr2024, Vol. 129 Issue 4, p1-23. 23p.
Subject Terms: *Ozone, *Climatology, *Trace gases, *Ozone layer, *Dust storms, Mars (Planet), Ice clouds
Abstract: The distribution of Mars ozone (O3) is well established; however, our knowledge on the dayside diurnal variation of O3 is limited. We present measurements of Mars O3 column abundances, spanning Mars Year (MY) 34 to the end of MY 36, by the Ultraviolet and VIsible Spectrometer (UVIS), part of the Nadir and Occultation for MArs Discovery (NOMAD) instrument, aboard the ExoMars Trace Gas Orbiter. UVIS provides the capability to measure dayside diurnal variations of O3 and for the first time, a characterization of the dayside diurnal variations of O3 is attempted. The observed O3 climatology for Mars Years (MY) 34–36 follows the established seasonal trends observed through previous O3 measurements. At aphelion, the equatorial O3 distribution is observed to be strongly correlated with the water ice distribution. We show that the early dust storm in MY 35 resulted in a near‐global reduction in O3 during northern spring and the O3 abundances remained 14% lower in northern summer compared to MY36. Strong latitudinal and longitudinal variation was observed in the diurnal behavior of O3 around the northern summer solstice. In areas with a weak O3 upper layer, O3 column abundance peaks in the mid‐morning, driven by changes in the near‐surface O3 layer. In regions with greater O3 column abundances, O3 is observed to gradually increase throughout the day. This is consistent with the expected diurnal trend of O3 above the hygropause and suggests that in these areas an upper O3 layer persists throughout the Martian day. Plain Language Summary: Ozone, a highly reactive gas, plays an important role in the chemical cycles of both carbon and hydrogen on Mars. As ozone is tightly correlated to the presence of the difficult to detect odd hydrogen species, measurement of the ozone distribution can provide vital insight into the Martian photochemistry. We present the ozone abundances measured by the UVIS spectrometer aboard the ExoMars Trace Gas Orbiter, spanning Mars years (MYs) 34–36 and attempt to characterize the daily variations in ozone. The ozone follows the expected seasonal trends, with the highest ozone abundances observed at polar regions in the spring, autumn and winter seasons of both hemispheres and very little ozone during southern summer, outside the northern polar latitudes. An enhancement in equatorial ozone during northern summer is observed, with MY 35 showing lower ozone abundances compared to MY 36, likely the effect of an early dust storm in MY 35 or the long‐term impact of the MY 34 global dust storm. In both years, the O3 distribution in northern summer appears to closely follow the water ice distribution and the observed daily cycle in ozone is shown to be highly sensitive to the presence of a high altitude ozone layer. Key Points: Dayside O3 column abundances on Mars between MY 34 (LS = 150°) and MY 36 have been obtained using the NOMAD‐UVIS instrumentOzone is strongly correlated with the presence of water ice clouds in the aphelion seasonDifferences between observed and modeled ozone diurnal variations points toward an under/overestimation of water ice condensation [ABSTRACT FROM AUTHOR]
Copyright of Journal of Geophysical Research. Planets is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: Climatology and Diurnal Variation of Ozone Column Abundances for 2.5 Mars Years as Measured by the NOMAD‐UVIS Spectrometer.
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  Data: <searchLink fieldCode="AR" term="%22Mason%2C+J%2E+P%2E%22">Mason, J. P.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<i> jon.mason@open.ac.uk</i><br /><searchLink fieldCode="AR" term="%22Patel%2C+M%2E+R%2E%22">Patel, M. R.</searchLink><relatesTo>1,2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Holmes%2C+J%2E+A%2E%22">Holmes, J. A.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Wolff%2C+M%2E+J%2E%22">Wolff, M. J.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Alday%2C+J%2E%22">Alday, J.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Streeter%2C+P%2E%22">Streeter, P.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Olsen%2C+K%2E+S%2E%22">Olsen, K. S.</searchLink><relatesTo>1,4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Brown%2C+M%2E+A%2E+J%2E%22">Brown, M. A. J.</searchLink><relatesTo>1,5</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Sellers%2C+G%2E%22">Sellers, G.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Marriner%2C+C%2E%22">Marriner, C.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Willame%2C+Y%2E%22">Willame, Y.</searchLink><relatesTo>6</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Thomas%2C+I%2E%22">Thomas, I.</searchLink><relatesTo>6</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Ristic%2C+B%2E%22">Ristic, B.</searchLink><relatesTo>6</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Daerden%2C+F%2E%22">Daerden, F.</searchLink><relatesTo>6</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Vandaele%2C+A%2E+C%2E%22">Vandaele, A. C.</searchLink><relatesTo>6</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Lopez‐Moreno%2C+J%2E‐J%2E%22">Lopez‐Moreno, J.‐J.</searchLink><relatesTo>7</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Bellucci%2C+G%2E%22">Bellucci, G.</searchLink><relatesTo>8</relatesTo> (AUTHOR)
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  Data: <searchLink fieldCode="JN" term="%22Journal+of+Geophysical+Research%2E+Planets%22">Journal of Geophysical Research. Planets</searchLink>. Apr2024, Vol. 129 Issue 4, p1-23. 23p.
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– Name: Abstract
  Label: Abstract
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  Data: The distribution of Mars ozone (O3) is well established; however, our knowledge on the dayside diurnal variation of O3 is limited. We present measurements of Mars O3 column abundances, spanning Mars Year (MY) 34 to the end of MY 36, by the Ultraviolet and VIsible Spectrometer (UVIS), part of the Nadir and Occultation for MArs Discovery (NOMAD) instrument, aboard the ExoMars Trace Gas Orbiter. UVIS provides the capability to measure dayside diurnal variations of O3 and for the first time, a characterization of the dayside diurnal variations of O3 is attempted. The observed O3 climatology for Mars Years (MY) 34–36 follows the established seasonal trends observed through previous O3 measurements. At aphelion, the equatorial O3 distribution is observed to be strongly correlated with the water ice distribution. We show that the early dust storm in MY 35 resulted in a near‐global reduction in O3 during northern spring and the O3 abundances remained 14% lower in northern summer compared to MY36. Strong latitudinal and longitudinal variation was observed in the diurnal behavior of O3 around the northern summer solstice. In areas with a weak O3 upper layer, O3 column abundance peaks in the mid‐morning, driven by changes in the near‐surface O3 layer. In regions with greater O3 column abundances, O3 is observed to gradually increase throughout the day. This is consistent with the expected diurnal trend of O3 above the hygropause and suggests that in these areas an upper O3 layer persists throughout the Martian day. Plain Language Summary: Ozone, a highly reactive gas, plays an important role in the chemical cycles of both carbon and hydrogen on Mars. As ozone is tightly correlated to the presence of the difficult to detect odd hydrogen species, measurement of the ozone distribution can provide vital insight into the Martian photochemistry. We present the ozone abundances measured by the UVIS spectrometer aboard the ExoMars Trace Gas Orbiter, spanning Mars years (MYs) 34–36 and attempt to characterize the daily variations in ozone. The ozone follows the expected seasonal trends, with the highest ozone abundances observed at polar regions in the spring, autumn and winter seasons of both hemispheres and very little ozone during southern summer, outside the northern polar latitudes. An enhancement in equatorial ozone during northern summer is observed, with MY 35 showing lower ozone abundances compared to MY 36, likely the effect of an early dust storm in MY 35 or the long‐term impact of the MY 34 global dust storm. In both years, the O3 distribution in northern summer appears to closely follow the water ice distribution and the observed daily cycle in ozone is shown to be highly sensitive to the presence of a high altitude ozone layer. Key Points: Dayside O3 column abundances on Mars between MY 34 (LS = 150°) and MY 36 have been obtained using the NOMAD‐UVIS instrumentOzone is strongly correlated with the presence of water ice clouds in the aphelion seasonDifferences between observed and modeled ozone diurnal variations points toward an under/overestimation of water ice condensation [ABSTRACT FROM AUTHOR]
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  Data: <i>Copyright of Journal of Geophysical Research. Planets is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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