Dust storm and electron density in the equatorial <i>D</i> region ionosphere of Mars: Comparison with Earth's ionosphere from rocket measurements in Brazil

Haider, S. A.; Batista, I. S.; Abdu, M. A.; Muralikrishna, P.; Shah, Siddhi Y.; Kuroda, Takeshi

doi:10.1002/2015ja021630

Cited by 10 publications

(7 citation statements)

References 18 publications

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“…In this season, as Mars approaches the Sun, increased solar irradiance and temperatures lead to a warmer and more circulated Martian atmosphere, which then lifts dust off the surface of Mars and causes the so-called dust storms. These dust storms have been previously shown to interact with the upper atmosphere and ionosphere of Mars in various ways, including the possibility of modulating the neutral densities and TEC [e.g., Wang and Nielsen, 2004;Mouginot et al, 2008;Liemohn et al, 2012;Withers, 2009;Withers and Pratt, 2013;Withers et al, 2015;Xu et al, 2014;Haider et al, 2015;Němec et al, 2015]. However, we do not draw any further conclusions on how the dust storms could directly impact the location of the Martian bow shock and leave such an investigation to a future study.…”

Section: Discussionmentioning

confidence: 86%

Annual variations in the Martian bow shock location as observed by the Mars Express mission

et al. 2016

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The Martian bow shock distance has previously been shown to be anticorrelated with solar wind dynamic pressure but correlated with solar extreme ultraviolet (EUV) irradiance. Since both of these solar parameters reduce with the square of the distance from the Sun, and Mars' orbit about the Sun increases by ∼0.3 AU from perihelion to aphelion, it is not clear how the bow shock location will respond to variations in these solar parameters, if at all, throughout its orbit. In order to characterize such a response, we use more than 5 Martian years of Mars Express Analyser of Space Plasma and EneRgetic Atoms (ASPERA‐3) Electron Spectrometer measurements to automatically identify 11,861 bow shock crossings. We have discovered that the bow shock distance as a function of solar longitude has a minimum of 2.39RM around aphelion and proceeds to a maximum of 2.65RM around perihelion, presenting an overall variation of ∼11% throughout the Martian orbit. We have verified previous findings that the bow shock in southern hemisphere is on average located farther away from Mars than in the northern hemisphere. However, this hemispherical asymmetry is small (total distance variation of ∼2.4%), and the same annual variations occur irrespective of the hemisphere. We have identified that the bow shock location is more sensitive to variations in the solar EUV irradiance than to solar wind dynamic pressure variations. We have proposed possible interaction mechanisms between the solar EUV flux and Martian plasma environment that could explain this annual variation in bow shock location.

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Section: Discussionmentioning

confidence: 86%

Annual variations in the Martian bow shock location as observed by the Mars Express mission

et al. 2016

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“…The lower‐resolution version of the MGCM has been validated against the observed zonal mean climatology (Kuroda et al, ) and applied for studies of baroclinic planetary wave activity (Kuroda et al, ), annular mode variability in the middle and high latitudes (Yamashita et al, ), equatorial semiannual oscillations (Kuroda et al, ), winter polar warmings during dust storms (Kuroda et al, ), and CO 2 snowfalls during northern polar winters (Kuroda et al, ). Recently, this model has been used for validating the temperature retrievals from the MGS radio occultations during the southern polar night (Noguchi et al, ), studying modulation of CO 2 clouds by stationary and transient waves (Noguchi et al, ), and exploring the influence of a global dust storm on the electron densities in the D region of the ionosphere (Haider et al, ).…”

Section: Methodsmentioning

confidence: 99%

Annual Cycle of Gravity Wave Activity Derived From a High‐Resolution Martian General Circulation Model

2019

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The paper presents results of simulations with a high‐resolution (equivalent to ∼67‐km grid size) Martian general circulation model (MGCM) from the surface up to the mesosphere for a full Martian year. The obtained climatology of the small‐scale disturbances can serve as a proxy for gravity waves (GWs) that are largely not resolved by MGCMs with conventional grid resolution and thus have to be parameterized. GW activity varies greatly with season and geographical location, which contradicts with the constant in space and time sources in the lower atmosphere adopted by GW parameterizations employed by coarse‐grid MGCMs. In particular, lower‐atmospheric GW activity is smaller in polar regions of the troposphere throughout all seasons, and the intensity is larger in southern spring and summer and in winter hemisphere at both solstices. In the mesosphere, the peak of GW activity shifts toward middle and high latitudes, and the interhemispheric symmetry is much larger compared to the lower atmosphere. The detailed climatology created in this study can be used for prescribing sources of GWs in parameterizations utilized by MGCMs as well as for validating the parameterizations in the middle and upper atmosphere.

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“…The regional dust storms occurred in different seasons of Mars at optical depth τ = 0.5 to 0.75 between L s ~0°–50°, 200°, and L s ~275°–350°. In this dust storm a large amount of dust lifted up into the atmosphere and formed two distinct layers at altitude range ~20–30 and ~45–65 km (Haider et al, ). These dust layers have been observed by CRISM and Mars Climate Sounder (MCS) onboard Mars Reconnaissance Orbiter (Guzewich et al, ; Heavens et al, ) (it should be noted that the dust optical depths obtained from SPICAM are generally larger than the results obtained from MER, MCS, and CRISM (Willame et al, )).…”

Section: Resultsmentioning

confidence: 99%

“…Recently, the high‐energy cosmic ray flux has been observed on the surface of Mars by the Radiation Assessment Detector (RAD) instrument onboard the Mars Science Laboratory (MSL; Ehresmann et al, ). We have not used this flux in our model because the RAD instrument observed mainly muon flux on the surface of Mars after attenuation of GCR through the atmosphere (Haider et al, ).…”

Section: Modelmentioning

confidence: 99%

“…In the present paper we have also calculated annual seasonal dependence of the production rates of O 3 + using energy loss model (Haider et al, , , , ) due to impact of galactic cosmic rays (GCR) in the dayside troposphere of Mars in presence and absence of dust storm during MY28 and MY29, respectively. These production rates can be used in future for the global modeling of the D region ionosphere of Mars.…”

Section: Introductionmentioning

confidence: 99%

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Effect of Dust Storm and GCR Impact on the Production Rate of O₃⁺ in MY 28 and MY 29: Modeling and SPICAM Observation

et al. 2019

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We have developed a seasonally dependent energy loss model to calculate the zonally averaged production rates of O 3 + due to impact of galactic cosmic rays in the dayside troposphere of Mars between solar longitudes (L s )~0°and 360°at low latitudes (2°N, 2°S, 25°N, and 25°S), midlatitudes (45°N and 45°S), and high latitudes (70°N and 70°S) in the Martian Year (MY) 28 and MY 29. We also represent the seasonal variability of zonally averaged ozone column density obtained from Mars Climate Database (MCD; Millour et al., 2014, https://hal.archives-ouvertes.fr/hal-01139592) during the daytime. These results are compared with the daytime observations of column ozone made by Spectroscopy for the Investigation of the Characteristics of the Atmosphere of Mars onboard Mars Express (MEX). At mid-to-high latitudes ozone column density is maximum in northern winter and minimum in southern summer. At low-to-middle latitudes (2°N-S, 25°N-S, and 45°N-S), the production rates of O 3 + represent a broad peak between altitudes 26 and 45 km in both hemispheres. The peak production rates are increasing up to L s = 47.5°and then stabilized at about 2.5 × 10 −8 cm −3 /s. At L s ≥ 47.5°the peak production rate of O 3 + starts decreasing until it disappeared after L s = 127.5°. A major dust storm occurred in MY 28 at L s~2 80°in southern latitudes (~25°-35°S). During the dust storm period, dust opacity, ozone column density, and O 3 + production rate on the surface of Mars were increased by a factor of~3.

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Dust storm and electron density in the equatorial D region ionosphere of Mars: Comparison with Earth's ionosphere from rocket measurements in Brazil

Cited by 10 publications

References 18 publications

Annual variations in the Martian bow shock location as observed by the Mars Express mission

Annual variations in the Martian bow shock location as observed by the Mars Express mission

Annual Cycle of Gravity Wave Activity Derived From a High‐Resolution Martian General Circulation Model

Effect of Dust Storm and GCR Impact on the Production Rate of O₃⁺ in MY 28 and MY 29: Modeling and SPICAM Observation

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Dust storm and electron density in the equatorial D region ionosphere of Mars: Comparison with Earth's ionosphere from rocket measurements in Brazil

Cited by 10 publications

References 18 publications

Annual variations in the Martian bow shock location as observed by the Mars Express mission

Annual variations in the Martian bow shock location as observed by the Mars Express mission

Annual Cycle of Gravity Wave Activity Derived From a High‐Resolution Martian General Circulation Model

Effect of Dust Storm and GCR Impact on the Production Rate of O3+ in MY 28 and MY 29: Modeling and SPICAM Observation

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Effect of Dust Storm and GCR Impact on the Production Rate of O₃⁺ in MY 28 and MY 29: Modeling and SPICAM Observation