The Martian Ionosphere in Regions of Crustal Magnetic Fields Paul Withers, Michael Mendillo, Dave Hinson DPS 2004, Louisville, Kentucky,

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Presentation transcript:

The Martian Ionosphere in Regions of Crustal Magnetic Fields Paul Withers, Michael Mendillo, Dave Hinson DPS 2004, Louisville, Kentucky, Abnormal electron density profiles are found over crustal magnetic anomalies in the southern hemisphere How does the martian magnetic field affect the ionosphere?

Normal ProfileAbnormal Profile “Abnormal” defined as:max | dN e /dz | / max (N e ) > 1 / 6 km Aim is to identify profiles with large changes in n over a short distance – extreme waviness. Exact definition is subjective and will probably be improved. Horizontal scale of measurement, sqrt(H R), is ~ 200 km

5 Normal Profiles5 Abnormal Profiles Compare 5 abnormal profiles to 5 normal profiles from same latitude/SZA/time population Much more variation exists within the abnormal subset Are abnormal profiles associated with geographic regions?

We thank to Jafar Arkani-Hamed for his magnetic field model + abnormal  normal

Magnetic Fields Can … Modify influx of energetic particles Modify plasma diffusion due to gravity, pressure Modify plasma transport by winds Relative size of ion-neutral collision frequency and ion gyrofrequency is critical – eB/m i in What happens when eB/m in is ~ 1? We are developing models to simulate these interactions

Some Fieldlines Regions of vertical fieldlines Regions of horizontal fieldlines Note that solar wind field is neglected Geometry changes over short distances

Conclusions Some ionospheric profiles over crustal magnetic anomalies are abnormal due to their extreme waviness It is important to understand interactions between the ionosphere and magnetic field because –The topology of the magnetic field of Mars is unique, having a small characteristic length scale –How have interactions between the ionosphere and magnetic field affected the loss of volatiles? –Do these interactions affect the energy and momentum balances of the neutral atmosphere?

Br at 400 km altitude, max value ~ 200 nT

NH examples, Chapman fit is good SH examples, Chapman fit is not good 65S, 12 noon, 80 SZA, strong winds close to boundary of winter polar night What are dynamics doing?