SEP 1F Ion and e- energy [keV] panels:

Ion and electron energies as measured by the Solar Energetic Particle Detector (SEP; Larson et al., 2015) onboard the NASA Mars Atmosphere and Volatile Evolution spacecraft (MAVEN; Jakosky et al., 2015; https://lasp.colorado.edu/maven/). The spectrograms show differential energy fluxes [keV/(cm2 s sr keV)] in color for the 20 keV to 6 MeV ions and 20 to 200 keV electrons.

SEP 1F ion and e- flux intensity panels:

Intensities of MAVEN/SEP ion and electron energies integrated over the energy ranges as labeled: ions: 20-100 keV, 100-900 keV, 1-6 MeV; electrons: 20-100 keV, 100-200 keV.

SWIA Energy [eV] panel:

Ion energy as measured by the MAVEN Solar Wind Ion Analyzer (SWIA; Halekas et al., 2015). The spectrogram shows the omni-directional differential energy flux in color, as a function of energy per charge and time, in 48 energy per charge bins. These energy spectra are produced by summing accumulated counts onboard over all instrument azimuthal and polar angles to produce a 48-element array of accumulated counts, and then converting to differential energy flux using the known instrument sensitivity. These onboard energy spectra should not be used for quantitative purposes since they do not include any angle-dependent relative sensitivity corrections. Their primary purpose is as a high-time-resolution diagnostic with continuous time coverage.

SWEA Energy [eV] panel:

Superthermal electron energies as measured by the MAVEN Solar Wind Electron Analyzer (SWEA; Mitchell et al., 2016). The colors show the differential electron energy fluxes [eV/(cm2 s sr eV)], which are averaged over SWEA's full field of view (FOV) of 360 x 120 deg at an energy range of 3-4600 eV.

The cadence of SEP, SWIA, and SWEA instruments are every between 2 and 8 sec, depending on these science products; however, the above panels are time-averaged by every 5 min to show the average behavior in response to the heliospheric disturbances.

Altitude [km] panel:

The MAVEN orbit is elliptical and precesses around Mars. Therefore, upstream solar wind observations are not routinely available. The spacecraft altitude is color coded according to the anticipated plasma regimes based on the Martian plasma boundary model (Trotignon et al., 2006). Details regarding the orbit geometry for a time frame of interest can be accessed through the MAVEN mission page: https://lasp.colorado.edu/maven/sdc/public/pages/plots/ql_orb/index.html

WIND = Upstream solar wind
SHEATH = Magnetosheath
PILEUP = Magnetic pileup region
EUV SHD = EUV Shadow

MAVEN/SWIA Nsw, Vsw and MAVEN/MAG IMF Brtn panels:

The orbit-averaged, upstream solar wind and IMF data obtained from the SWIA and the MAVEN Magnetometer (MAG;Connerney et al., 2015) instruments, respectively, are determined according to an algorithm developed by Dr. Halekas (Halekas et al., 2017). The IMF data shown are converted into the RTN (Radial-Tangential-Normal) coordinates system. The synthesized upstream solar wind data sets, with the IMF vector data in the Mars-Sun-Orbit (MSO) coordinates, based on publicly released Level 2 data from SWIA and MAG, along with additional details and references may be obtained at https://homepage.physics.uiowa.edu/~jhalekas/drivers.html.

Data Usage:

These data are quick look data and should not be used for analysis or publication. Please use the official MAVEN SEP, SWIA, SWEA, and MAG data products located at the Planetary Data System (PDS): https://pds-ppi.igpp.ucla.edu/mission/MAVEN/MAVEN. These data are also available at the Space Physics Data Facility (SPDF): https://cdaweb.gsfc.nasa.gov/cgi-bin/eval1.cgi?index=sp_phys&group=MAVEN

References: