ABSTRACT LIST INTERNATIONAL VENUS WORKSHOP
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INTERNATIONAL VENUS WORKSHOP
ABSTRACT LISTMonday, 10th June
Schedule Author Title
9:00 - 13:00 SWT
9:00 - 13:00 Science Working Team meeting (only for the Venus Express team members)
14:30 Session Surface/Interior
14:30 - 15:00 Stofan Venus: Earth’s (Neglected) Twin (Invited)
15:00 - 15:15 Mueller Search for active lava flows with VIRTIS on Venus Express
Venus surface geology from near infrared night side Venus Monitoring Camera
15:15 - 15:30 Shalygin
images
Diverse Geologic Settings of Recent Volcanism on Venus and
15:30 - 16:00 Smrekar
Implications for the Interior (Invited)
16:00 - 16:30 Coffee
16:30 Session Surface/Interior
16:30 - 17:00 Sotin Are terrestrial exoplanets Earth-like, Venus-like, or different? (Invited)
17:00 - 17:15 Ghail The influence of rheology and volatiles on the geology of Venus
17:15 - 17:45 Russell Venus and Planetary Magnetism (Invited)
Large-scale magnetic flux ropes in low-altitude ionosphere of Venus: planetary
17:45 - 18:00 Luhmann
origin or solar wind origin
18:00 - 18:15 Discussion of Surface/Interior/Magnetism
18:15 - 19:45 Poster session 1
Tuesday, 11th June
Schedule Author Title
9:00 Session Plasma & Induced Magnetosphere
9:00 - 9:30 Zhang Physics of Induced Magnetosphere (Invited)
Comparative Plasma Interactions and their Effects at Venus, Mars and
9:30 - 10:00 Luhmann
Titan (Invited)
10:00 - 10:15 Barabash How the near-Venus space affects the planet
10:15 - 10:30 Stenberg Ion escape from Venus
Dependence of O+ escape rate from the Venusian upper atmosphere on IMF
10:30 - 10:45 Masunaga
directions: ASPERA-4 observations
Comparisons of Venus Express measurements with an MHD model of O+ ion
10:45 - 11:00 McEnulty
flows: Implications for atmosphere escape measurements
11:00 - 11:30 Coffee
11:30 Session Plasma & Induced Magnetosphere
Solar Wind energy and momentum transfer - Effects on the Venus polar
11:30 - 11:45 Lundin
thermosphere
The plasma vortex in the Venusian plasma tail. Steady-state reconnection or fluid
11:45 - 12:00 Fedorov
motion?
12:00 - 12:15 Nordheim Cosmic ray ionization in the Venusian atmosphere from Monte Carlo modelling
12:15 - 12:30 Dubinin Ionospheric magnetic fields and currents at Mars and Venus
12:30 - 12:45 Vasko Fine structure of the Venus current sheet
12:45 - 13:00 Coates Ionospheric photoelectron observations at Venus
13:00 - 13:15 Gray A survey of Hot Flow Anomalies at Venus
13:15 - 13:30 Russell The Implications of the Observed Evolution of the Co-Orbiting Material in 2201
PROGRAM – PAGE AOljato’s Orbit Observed by PVO and VEX
13:30 Lunch
15:30 Etna excursion
Wednesday, 12th June
Schedule Author Title
9:00 Session Dynamics & Structure
Venus GCM modelling: current status and perspectives in the light of Venus
9:00 - 9:25 Lebonnois
Express datasets (Invited)
9:25 - 9:50 Rodin Non-hydrostatic general circulation model of the Venus atmosphere (Invited)
9:50 - 10:05 Takagi Structures and generation mechanisms of the Venus atmospheric superrotation
Baroclinic modes in the Venus atmosphere simulated by AFES (Atmospheric GCM For the
10:05 - 10:20 Sugimoto
Earth Simulator)
10:20 - 10:35 Limaye Global Vortex Circulation on Venus - an assessment from Venus Express Observations
Measurements of Venus winds from ultraviolet, visible and near infrared images with
10:35 - 10:50 Hueso
VIRTIS on Venus Express
10:50 - 11:05 Bertaux Atmospheric Oscillation in the atmosphere of Venus: the Cupido effect
11:05 - 11:30 Coffee
11:30 Session Dynamics & Structure
Variations of the radiative forcing induced by the cloud top structure changes of the
11:30 - 11:45 Lee
Venus mesosphere
11:45 - 12:00 Grassi Thermal Structure of Venus Mesosphere as Observed by VIRTIS - Venus Express
Thermal structure of the Venus mesosphere from remote sensing in the infrared spectral
12:00 - 12:15 Zasova
range (VIRA II improvement)
12:15 - 12:30 Tellmann The VeRa Radio Occultation Data Base: Atmosphere and Ionosphere (Invited)
Waves in the Venus Atmosphere detected by the Venus Express Radio Science
12:30 - 12:45 Tellmann
Experiment VeRa (Invited)
12:45 - 13:00 Migliorini Gravity waves in the Venus upper atmosphere, modelled on VIRTIS/Venus Express data
13:00 - 14:30 Lunch
14:30 Session Upper Mesosphere/Lower Thermosphere
14:30 - 14:45 Piccialli Thermal structure of the upper atmosphere of Venus with SPICAV/VEx data
CO2 rotational temperatures compared to hydrostatic temperatures obtained with the
14:45 - 15:00 Mahieux
SOIR instrument on board VEx
Incorporation of a gravity wave momentum deposition parameterization into the Venus
15:00 - 15:15 Zalucha
thermosphere general circulation Model (VTGCM)
Retrieval of temperature and carbon monoxide from the 4.7um limb non-LTE emission of
15:15 - 15:30 Lopez-Valverde
the upper atmosphere measured by VIRTIS/Venus Express
Earth based Doppler-wind and temperature measurements in Venus upper atmosphere
15:30 - 15:45 Sornig
using the infrared heterodyne spectrometer THIS
Doppler Winds Mapped around the Lower Thermospheric Terminator of Venus: JCMT
15:45 - 16:00 Clancy
Observations of the 2012 Solar Transit
16:00 - 16:30 Coffee
16:30 Session Upper Mesosphere/Lower Thermosphere
Venus night side measurements of winds at 115 km altitude from NO bright patches
16:30 - 16:45 Bertaux
tracking
16:45 - 17:00 Stiepen Venus nitric oxide nightglow distribution: a clue to thermospheric dynamics
17:00 - 17:15 Zasova The O2 nightglow from VIRTIS-M VEX measurements
17:15 - 17:30 Gérard Latitudinal variations of the altitude of the Venus O2 airglow observed with VIRTIS-M: a
PROGRAM – PAGE Bsignature of dynamical processes in the upper atmosphere
17:30 - 17:45 Jain Modelling of ultraviolet and visible dayglow emissions on Venus
17:45 - 18:00 Clarke Coordinated Sounding Rocket, HST, and SPICAV Observations of Venus in Nov. 2013
18:00 - 18:15 Discussion of airglow and dynamics
18:15 -19:45 Poster session 2
Thursday, 13th June
Schedule Author Title
9:00 Session Chemistry & Composition
Ground-based observations of minor species on Venus using infrared
9:00 - 9:15 Encrenaz
spectroscopy (Invited)
9:15 - 9:30 Encrenaz Sulfur and water mapping in the mesosphere of Venus
9:30 - 9:45 Marcq Measurements of minor species at cloud top level
Water vapor and the cloud top variations in the Venus’ mesosphere from SPICAV
9:45 - 10:00 Fedorova
observations
10:00 - 10:15 McGouldrick Re-analysis of Pioneer Venus SO2 measurements
Assessing An Impact Hypothesis for Upper Atmosphere Abundance Variations on
10:15 - 10:30 Grinspoon
Venus
10:30 - 11:00 Coffee
11:00 Session Chemistry & Composition
Positive Correlation of SO, SO2 in the Dayside Venus Mesosphere: Identification of
11:00 - 11:15 Sandor
Diurnal SOx Partitioning from JCMT Submm Spectroscopy
Temporal, Spatial Variation of HCl in the Venus Mesosphere, based upon Submm
11:15 - 11:30 Sandor
Spectroscopic Observations with JCMT
Trace gases in the mesosphere and lower thermosphere of Venus from
11:30 - 11:45 Vandaele
SOIR/VEX (Invited)
11:45 - 12:00 Vandaele Contribution of the SOIR/VEX instrument to VIRA II (Invited)
12:00 Session Clouds & Hazes
12:00 - 12:30 Wilquet SPICAV-SOIR mesospheric aerosols observations and modeling (Invited)
12:30 - 12:45 Titov/Markiewicz Venus cloud morphology: monitoring by the VMC/ Venus Express camera continued
Physical properties of particles in the upper clouds of Venus from the IR and UV
12:45 - 13:00 Petrova
images taken by VMC/VEx at small phase angles
13:00 - 14:30 Lunch
14:30 Session Clouds & Hazes
Temporal variation of UV reflectivity of Venus: VEX/VMC data analysis
14:30 - 15:00 Hashimoto
(Invited)
15:00 - 15:15 Esposito Causes of the bright and dark features at the Venus cloud tops
15:15 - 15:30 Satoh On the origin of the 1-micron contrast features in Venus clouds
Modeling the clouds on Venus: model development and improvement of a nucleation
15:30 - 15:45 Maattanen
parameterization
15:45 - 16:00 Imamura Latitudinal and local time dependence of Venus's cloud-level convection
16:00 - 16:15 Ignatiev Cloud top variations from Venus Express measurements (Invited)
Venus Clouds: Input to VIRA II model from Venus Express and Venera 15
16:15 - 16:30 Ignatiev
measurements (Invited)
16:30 - 16:45 Discussion of chemistry and clouds
16:45 - 17:15 Coffee
17:15 Session Lab-based
17:15 - 17:40 Helbert High temperature spectroscopy at the Planetary Emissivity Laboratory in
PROGRAM – PAGE Csupport of present and future Venus missions" (Invited)
17:40 - 18:05 Slanger Long-lived Emitters in the Atmospheres of the Terrestrial Planets (Invited)
Experimental and theoretical studies of CO2 infrared absorption continua
18:05 - 18:30 Hartmann
(Invited)
18:30 - 18:45 Kohler Experimental Stability of Tellurium: Implications for the Venusian Radar Anomalies
Experimental set-up to study optical properties of gases at typically planetary
18:45 - 19:00 Stefani
conditions
Carbon dioxide collision induced absorption in the 1.18 micron atmospheric window of
19:00 - 19:15 Snels
Venus
20:00 Team dinner
Friday, 14th June
Schedule Author Title
9:00 Session Evolution
9:00 - 9:25 Moresi The influence of surface conditions on global mantle evolution (Invited)
9:25 - 9:40 Gillmann Long term evolution of Venus through Mantle/Atmosphere coupling
Thermal evolution of an early magma ocean in interaction with the atmosphere:
9:40 - 9:55 Lebrun
conditions for the condensation of a water ocean
9:55 - 10:10 Marcq Early evolution of telluric atmospheres in the magma ocean stage
10:10 - 10:25 Taylor Volcanism and Climate on Venus: An Updated Model
New calculations of the runaway greenhouse limit: bad news for early
10:25 - 10:50 Goldblatt
Venus and future Earth (Invited)
The origin and early evolution of Venus, Earth and Mars: Clues from bulk properties
10:50 - 11:05 Baines
and the abundances and isotopic ratios of noble and light gases
11:05 - 11:30 Coffee
11:30 Future
11:30 - 11:45 Nakamura Japan/Akatsuki report
11:45 - 12:00 Zasova Russia/Venera-D report
12:00 - 12:15 Limaye/Baines U.S./VEXAG report
12:15 - 12:30 Drossart Future Venus IR observation plans
12:30 - 12:45 All ISSI/EuroVenus/other reports
12:45 - 13:00 Taylor Venus III book discussions
13:00 - 13:15 Zasova VIRA II discussion
13:15 - 13:30 Wilson Future VEx science plan
13:30 - 14:00 All Discussion
14:00 End
PROGRAM – PAGE DGROUP 1 POSTER – MON‐WED
Author Title
Cochrane Errors and Artifacts in the Magellan Imagery of the Surface of Venus
Nunes Stereo-Derived Topography To Aid Emissivity Estimates at Tesserae on Venus
A global comparison between VeRa radio science observations of the Venus dayside
Peter
ionosphere and the IonA model
ULF and ELF Electromagnetic Waves in the Venus Ionosphere: Separating Atmospheric and
Russell
Magnetosheath Sources
Stenberg Solar wind precipitation on Venus
Molaverdikhani A new dawn-dusk asymmetry in the photoelectron flux of Venus’s Ionosphere
Ogohara Limb fitting and cloud tracking for the study of the Venus atmosphere
Mesospheric Temperature at Terminator using SDO/HMI Aureole Photometry, DST/FIRS
Widemann
CO2 absorption spectroscopy and comparison with Venus Express
Ando Vertical structure of the Venus vortex
Temperature variation of the cloud top of Venus obtained by photometry observation by LIR
Fukuhara
onboard Akatsuki
Gravity waves in Venus mesosphere observed by the Venus Monitoring Camera on board
Piccialli
Venus Express
Marinangeli Polar Vortex: a common element of the Earth and Venus
Peralta Towards a general classification of atmospheric waves on Venus
Yamamoto Simulation of Venus’ polar vortex in the presence of diurnal thermal tide
Venus cloud tops winds with ground-based Doppler velocimetry and comparison with cloud
Machado
tracking method
The time evolution of O2(a1Δ) individual observations acquired by VIRTIS-M on board Venus
Soret
Express
The variable upper atmosphere of Venus - data from drag and torque measurements by
Svedhem
Venus Express
Mapping the lower thermosphere of Venus using VIRTIS/VEx Nadir non-LTE observations at
López-Valverde
4.3 um
Visible and Infrared nightglow investigation in the Venus atmosphere by means of VIRTIS on
Migliorini
Venus Express
García-Muñoz Global imaging of the Venus O2 visible nightglow with the Venus Monitoring Camera
Gray The Effect of Coronal Mass Ejections and Solar Flares on the Venusian Nightglow
Mt. Etna and the Eistla volcanoes: Comparative studies to constrain venusian volcano
Anderson
evolution and flow emplacement
Temperatures in Venus' Lower Thermosphere: Comparison of VTGCM and SOIR Profiles at
Bougher / Parkinson
the Terminator
PROGRAM – PAGE EGROUP 2 POSTER – WED‐FRI
Author Title
Observations of the near-IR nightside windows of Venus during Maxwell Montes transits by
Fedorova
SPICAV IR onboard Venus Express
Iwagami Ground-based IR observation of oxygen isotope ratios in the Venus atmosphere
Abundance of sulfuric acid vapor in the Venus atmosphere derived from the Venus Express Radio
Oschlisniok
Science Experiment VeRa
Cottini Water vapor near the cloud tops of Venus from VIRTIS Venus Express day side data
Lorenz On the Possibility of Gamma Ray Flashes from Venusian Lightning
Mills Modeling and observations of mesospheric sulfur chemistry
Robert Spectral inventory of the SOIR spectra onboard Venus Express
Stolzenbach Three-dimensional modelling of Venus photochemistry
Jessup Variations in Venus’ cloud top SO2 and SO gas density with latitude and time of day
Politi VIRTIS-VEX data analysis for the study of the Venus
Progress in a refined calibration of the Venus Express VIRTIS-M instrument with application to
Carlson
Venus’s ultraviolet absorber
Enomoto Venusian upper hazes observed by Imaging-Polarimetry system HOPS
Latitudinal cloud structure in the Venusian northern hemisphere evaluated from Venus
Kuroda
Express/VIRTIS observations
Rossi Study of Venus cloud layers by polarimetry using SPICAV/VEx
Takagi High-altitude source for the Venus’ upper haze found by SOIR/Venus Express
Simulation of the formation, evaporation and transport of sulfuric acid clouds on Venus using a
Takeshi
general circulation model
Planetary Radio Interferometry and Doppler Experiments for current and future Venusian
Cimo
missions
Molera Calves Interplanetary scintillations study retrieved from Venus Express communications signal
Pluchino Using Venus Express to perform sounding experiments on lunar ionosphere
A compact, Low Power Tunable Laser Spectrometer for Trace Gas Measurement in the Venus
Rafkin
Atmosphere
Rodin A compact, lightweight infrared heterodyne spectrometer for studies of Venus atmosphere
Perez-Hoyos Analysis of MESSENGER/MASCS data during second Venus flyby
PROGRAM – PAGE FIndex
Authors Title Page
Anderson Mt. Etna and the Eistla volcanoes: Comparative studies to constrain venusian volcano
48
evolution and flow emplacement
Ando Vertical structure of the Venus vortex 42
Baines The origin and early evolution of Venus, Earth and Mars: Clues from bulk properties
and the abundances and isotopic ratios of noble and light gases 36
Barabash How the near-Venus space affects the planet 5
Bertaux Atmospheric Oscillation in the atmosphere of Venus: the Cupido effect 12
Bertaux Venus night side measurements of winds at 115 km altitude from NO bright patches
19
tracking.
Bougher / Parkinson Temperatures in Venus' Lower Thermosphere: Comparison of VTGCM and SOIR
48
Profiles at the Terminator
Carlson Progress in a refined calibration of the Venus Express VIRTIS-M instrument with
53
application to Venus’s ultraviolet absorber
Cimo Planetary Radio Interferometry and Doppler Experiments for current and future
56
Venusian missions
Clancy Doppler Winds Mapped around the Lower Thermospheric Terminator of Venus: JCMT
19
Observations of the 2012 Solar Transit
Clarke Coordinated Sounding Rocket, HST, and SPICAV Observations of Venus in Nov. 2013 21
Coates Ionospheric photoelectron observations at Venus 8
Cochrane Errors and Artifacts in the Magellan Imagery of the Surface of Venus 39
Collinson A survey of Hot Flow Anomalies at Venus 9
Cottini Water vapor near the cloud tops of Venus from VIRTIS Venus Express day side data 51
Drossart Future Venus IR observation plans 38
Dubinin Ionospheric magnetic fields and currents at Mars and Venus 8
Encrenaz Ground-based observations of minor species on Venus using infrared spectroscopy 23
Encrenaz Sulfur and water mapping in the mesosphere of Venus 23
Enomoto Venusian upper hazes observed by Imaging-Polarimetry system HOPS 54
Esposito Causes of the bright and dark features at the Venus cloud tops 28
Fedorov The plasma vortex in the Venusian plasma tail. Steady-state reconnection or fluid
7
motion?
Fedorova Water vapor and the cloud top variations in the Venus’ mesosphere from SPICAV
24
observations
Fedorova Observations of the near-IR nightside windows of Venus during Maxwell Montes
transits by SPICAV IR onboard Venus Express 50
Fukuhara Temperature variation of the cloud top of Venus obtained by photometry observation
42
by LIR onboard Akatsuki
García-Muñoz Global imaging of the Venus O2 visible nightglow with the Venus Monitoring Camera 47
Gérard Latitudinal variations of the altitude of the Venus O2 airglow observed with VIRTIS-
M: a signature of dynamical processes in the upper atmosphere 21
Ghail The influence of rheology and volatiles on the geology of Venus 3
Gillmann Long term evolution of Venus through Mantle/Atmosphere coupling. 34
Goldblatt New calculations of the runaway greenhouse limit: bad news for early Venus and
35
future Earth
Grassi Thermal Structure of Venus Mesosphere as Observed by VIRTIS - Venus Express 13
Gray The Effect of Coronal Mass Ejections and Solar Flares on the Venusian Nightglow 47
Grinspoon Assessing An Impact Hypothesis for Upper Atmosphere Abundance Variations on
25
Venus
Hartmann Experimental and theoretical studies of CO2 infrared absorption continua 32
Hashimoto Temporal variation of UV reflectivity of Venus: VEX/VMC data analysis 28
INDEX ‐ PAGE IHelbert High temperature spectroscopy at the Planetary Emissivity Laboratory in support of
31
present and future Venus missions"
Hueso Measurements of Venus winds from ultraviolet, visible and near infrared images with
12
VIRTIS on Venus Express
Ignatiev Cloud top variations from Venus Express measurements 30
Ignatiev Venus Clouds: Input to VIRA II model from Venus Express and Venera 15
30
measurements.
Imamura Latitudinal and local time dependence of Venus's cloud-level convection 29
Iwagami Ground-based IR observation of oxygen isotope ratios in the Venus atmosphere 50
Jain Modelling of ultraviolet and visible dayglow emissions on Venus 21
Jessup Variations in Venus’ cloud top SO2 and SO gas density with latitude and time of day 53
Kohler Experimental Stability of Tellurium: Implications for the Venusian Radar Anomalies 32
Kuroda Latitudinal cloud structure in the Venusian northern hemisphere evaluated from
Venus Express/VIRTIS observations 54
Lebonnois Venus GCM modelling: current status and perspectives in the light of Venus Express
10
datasets
LeBrun Thermal evolution of an early magma ocean in interaction with the atmosphere:
conditions for the condensation of a water ocean 34
Lee Variations of the radiative forcing induced by the cloud top structure changes of the
13
Venus mesosphere
Limaye Global Vortex Circulation on Venus - an assessment from Venus Express
11
Observations
Limaye/Baines U.S. / VEXAG report 37
Lopez-Valverde Retrieval of temperature and carbon monoxide from the 4.7um limb non-LTE
18
emission of the upper atmosphere measured by VIRTIS/Venus Express
López-Valverde Mapping the lower thermosphere of Venus using VIRTIS/VEx Nadir non-LTE
46
observations at 4.3 um
Lorenz On the Possibility of Gamma Ray Flashes from Venusian Lightning 51
Luhmann Large-scale magnetic flux ropes in low-altitude ionosphere of Venus: planetary origin
3
or solar wind origin
Luhmann Comparative Plasma Interactions and their Effects at Venus, Mars and Titan 5
Lundin Solar Wind energy and momentum transfer - Effects on the Venus polar
7
thermosphere
Maattanen Modeling the clouds on Venus: model development and improvement of a nucleation
29
parameterization
Machado Venus cloud tops winds with ground-based Doppler velocimetry and comparison with
44
cloud tracking method
Mahieux CO2 rotational temperatures compared to hydrostatic temperatures obtained with the
17
SOIR instrument on board VEx
Marcq Measurements of minor species at cloud top level 24
Marcq Early evolution of telluric atmospheres in the magma ocean stage 35
Marinangeli Polar Vortex: a common element of the Earth and Venus 43
Masunaga Dependence of O+ escape rate from the Venusian upper atmosphere on IMF
6
directions: ASPERA-4 observations
McEnulty Comparisons of Venus Express measurements with an MHD model of O+ ion flows:
Implications for atmosphere escape measurements 6
McGouldrick Re-analysis of Pioneer Venus SO2 measurements 25
Migliorini Gravity waves in the Venus upper atmosphere, modelled on VIRTIS/Venus Express
16
data
Migliorini Visible and Infrared nightglow investigation in the Venus atmosphere by means of
46
VIRTIS on Venus Express
Mills Modeling and observations of mesospheric sulfur chemistry 52
Molaverdikhani A new dawn-dusk asymmetry in the photoelectron flux of Venus’s Ionosphere 41
Molera Calves Interplanetary scintillations study retrieved from Venus Express communications
56
signal
INDEX ‐ PAGE IIMoresi The influence of surface conditions on global mantle evolution 34
Mueller Search for active lava flows with VIRTIS on Venus Express 1
Nakamura Japan / Akatsuki report 36
Nordheim Cosmic ray ionization in the Venusian atmosphere from Monte Carlo modelling 7
Nunes Stereo-Derived Topography To Aid Emissivity Estimates at Tesserae on Venus 39
Ogohara Limb fitting and cloud tracking for the study of the Venus atmosphere 41
Oschlisniok Abundance of sulfuric acid vapor in the Venus atmosphere derived from the Venus
Express Radio Science Experiment VeRa 50
Peralta Towards a general classification of atmospheric waves on Venus 44
Perez-Hoyos Analysis of MESSENGER/MASCS data during second Venus flyby 58
Peter A global comparison between VeRa radio science observations of the Venus dayside
39
ionosphere and the IonA model
Petrova Physical properties of particles in the upper clouds of Venus from the IR and UV
images taken by VMC/VEx at small phase angles 28
Piccialli Thermal structure of the upper atmosphere of Venus with SPICAV/VEx data 16
Piccialli Gravity waves in Venus mesosphere observed by the Venus Monitoring Camera on
43
board Venus Express
Pluchino Using Venus Express to perform sounding experiments on lunar ionosphere 57
Politi VIRTIS-VEX data analysis for the study of the Venus 53
Rafkin A compact, Low Power Tunable Laser Spectrometer for Trace Gas Measurement in
57
the Venus Atmosphere
Robert Spectral inventory of the SOIR spectra onboard Venus Express 52
Rodin Non-hydrostatic general circulation model of the Venus atmosphere 10
Rodin A compact, lightweight infrared heterodyne spectrometer for studies of Venus
57
atmosphere
Rossi Study of Venus cloud layers by polarimetry using SPICAV/VEx 55
Russell Venus and Planetary Magnetism 3
Russell The Implications of the Observed Evolution of the Co-Orbiting Material in 2201
9
Oljato’s Orbit Observed by PVO and VEX
Russell ULF and ELF Electromagnetic Waves in the Venus Ionosphere: Separating
40
Atmospheric and Magnetosheath Sources
Sandor Positive Correlation of SO, SO2 in the Dayside Venus Mesosphere: Identification of
Diurnal SOx Partitioning from JCMT Submm Spectroscopy 25
Sandor Temporal, Spatial Variation of HCl in the Venus Mesosphere, based upon Submm
26
Spectroscopic Observations with JCMT
Satoh On the origin of the 1-micron contrast features in Venus clouds 29
Shalygin Venus surface geology from near infrared night side Venus Monitoring Camera
1
images
Slanger Abstract Nr. O-014, Slanger, Tom, Long-lived Emitters in the Atmospheres of the
31
Terrestrial Planets
Smrekar Diverse Geologic Settings of Recent Volcanism on Venus and Implications for the
2
Interior
Snels Carbon dioxide collision induced absorption in the 1.18 micron atmospheric window
33
of Venus
Soret The time evolution of O2(a1Δ) individual observations acquired by VIRTIS-M on
45
board Venus Express
Sornig Earth based Doppler-wind and temperature measurements in Venus upper
atmosphere using the infrared heterodyne spectrometer THIS 18
Sotin Are terrestrial exoplanets Earth-like, Venus-like, or different ? 2
Stefani Experimental set-up to study optical properties of gases at typically planetary
33
conditions
Stenberg Ion escape from Venus 6
INDEX ‐ PAGE IIIStenberg Solar wind precipitation on Venus 40
Stiepen Venus nitric oxide nightglow distribution: a clue to thermospheric dynamics 20
Stofan Venus: Earth’s (Neglected) Twin 1
Stolzenbach Three-dimensional modelling of Venus photochemistry 52
Sugimoto Baroclinic modes in the Venus atmosphere simulated by AFES (Atmospheric GCM For
11
the Earth Simulator)
Svedhem The variable upper atmosphere of Venus - data from drag and torque measurements
45
by Venus Express
Takagi Structures and generation mechanisms of the Venus atmospheric superrotation 11
Takagi High-altitude source for the Venus’ upper haze found by SOIR/Venus Express 55
Takeshi Simulation of the formation, evaporation and transport of sulfuric acid clouds on
55
Venus using a general circulation model
Taylor Volcanism and Climate on Venus: An Updated Model 35
Taylor Venus III book discussion 38
Tellmann The VeRa Radio Occultation Data Base: Atmosphere and Ionosphere 14
Tellmann Waves in the Venus Atmosphere detected by the Venus Express Radio Science
15
Experiment VeRa
Titov / Markiewicz Venus cloud morphology: monitoring by the VMC/ Venus Express camera continued 27
Vandaele Trace gases in the mesosphere and lower thermosphere of Venus from SOIR/VEX 26
Vandaele Contribution of the SOIR/VEX instrument to VIRA II 26
Vasko Fine structure of the Venus current sheet 8
Widemann Mesospheric Temperature at Terminator using SDO/HMI Aureole Photometry,
41
DST/FIRS CO2 absorption spectroscopy and comparison with Venus Express
Wilquet SPICAV-SOIR mesospheric aerosols observations and modelling 27
Yamamoto Simulation of Venus’ polar vortex in the presence of diurnal thermal tide 44
Zalucha Incorporation of a gravity wave momentum deposition parameterization into the
Venus thermosphere general circulation Model (VTGCM) 17
Zasova Thermal structure of the Venus mesosphere from remote sensing in the infrared
14
spectral range (VIRA II improvement)
Zasova The O2 nightglow from VIRTIS-M VEX measurements 20
Zhang Physics of Induced Magnetosphere 5
INDEX ‐ PAGE IVORAL CONTRIBUTIONS
ORAL CONTRIBUTIONMonday, 10 June
Abstract Nr. 26
Venus: Earth’s (Neglected) Twin
Stofan, Ellen, Proxemy Research
Venus, so similar in size and composition to Earth, has a diverse and complex surface that has been
studied by spacecraft for over half a century, starting with the flyby of Mariner 2 in 1962. The Venera,
Vega, Pioneer Venus, Magellan, and now Venus Express missions have led to an increased
understanding of the surface and interior that lies under Venus’s clouds, and what this surface implies
about the planet’s evolution. From tesserae to coronae to volcanoes to mountain ranges and fracture
belts, analysis of the geologic features on the surface of Venus provide clues to its interior evolution.
The ~11 hotspot rises on Venus provide a window into interior processes, and indicate that the planet
is still active geologically. However, while our knowledge about Venus has greatly increased, the range
of theories to explain what we see remains quite large, and likley will remain so until future
investigations are conducted at the surface and in orbit around Venus. As we search beyond our own
solar system for Earth-like planets, it becomes more critical to understand why Earth’s twin is so
different and what it can tell us about Earth’s past and future.
Abstract Nr. 83
Search for active lava flows with VIRTIS on Venus Express
Mueller, Nils, Institute of Planetary Research, German Aerospace Center (DLR)
The VIRTIS instrument on Venus Express observes thermal emission from the surface of Venus at 1
µm wavelength and thus would detect sufficiently bright incandescent lava flows. No eruptions were
detected in the observations between April 2006 and October 2008. Models of the cooling of lava flows
on Earth are adapted to Venus ambient conditions to predict thermal emission based on effusion rate.
Taking into account the blurring of surface thermal emission by the atmosphere, the VIRTIS images
would detect eruptions with effusion rates above 500 to 1000 m3/s. Assuming the average eruption
volume and effusion rate distribution of Venus' lava flows is similar to that of the Hawaiian volcanoes
Mauna Loa and Kilauea, a typical VIRTIS observation would detect 4% to 10% of all lava flows within
its field of view and the whole data set is expected to lead to 0.02 detected eruptions per 1 km3 of
lava effused per year. Thus the VIRTIS data can constrain the rate of volcanism on Venus to be less
than about 100 km3/yr, at least a factor of 10 higher than existing constraints and the terrestrial value
of 4 km3/yr. While VIRTIS data does not place new constraints, the analysis shows that dedicated
volcano monitoring at Venus is feasible. There remains a large uncertainty because of the unknown
style of volcanism and the not well understood role of wind in lava surface cooling, but it could be
significantly reduced by analysis of high resolution radar images of flow fields and altimetry resolving
the thickness of flows.
Abstract Nr. 57
Venus surface geology from near infrared night side Venus Monitoring Camera images
Shalygin Eugene, Max-Planck Institute für Sonnensystemforschung; Basilevsky Alexander, Max-Planck
Institute für Sonnensystemforschung; Markiewicz Wojciech J., Max-Planck Institute für
Sonnensystemforschung; Titov Dmitrij, ESA-ESTEC
We analyse night-time near infra-red thermal emission images of the Venus surface obtained with the
1-µm channel of the VMC onboard Venus Express. We consider if SOME terrains have the different
emissivity (and thus mineralogic composition) in comparison to the surrounding basaltic plains.
Retrieved emissivity of tessera surface material is lower than that of relatively fresh supposedly
MONDAY, 10 JUNE ‐ PAGE 1basaltic lavas of plains and volcanic edifices. This is consistent with the hypothesis that the tessera
material may be felsic. We found a possible decrease of the emissivity at the top of Tuulikki Mons
volcano which, if real, may be due to different (more felsic?) composition of volcanic products on the
volcano summit comparing to its slopes.
We simulated lava eruptions to access the possibility to detect ongoing volcanic activity. Simulations
showed that 1 square km lava flows should be marginally seen by VMC. 2-3 square km lava fields are
visible on the plains and 4-5 square km - even in deep rift zones.
Typical individual lava flows on Tuuliki Mons are large enough to produce contrasts of 1000% between
them and surroundings in VMC images. But typical lava flows from shield volcanoes on Earth often
have been being formed during weeks to months and the instantaneous size of the hot flow surface
was usually much smaller. Thus the detection probability is significantly lower, but it is far from being
negligible.
Abstract Nr. 120
Diverse Geologic Settings of Recent Volcanism on Venus and Implications for the Interior
Smrekar, Jet Propulsion Laboratory, NASA/Caltech
Analysis of VIRTIS data identified four primary areas of high 1-micron surface emissivity, interpreted
as evidence of recent volcanism. Prior analysis of gravity and topography of 3 of the 4 areas, as well
as interpretation of their surface geology, indicated that they are likely to be supported by a mantle
plume, or hotspots. New analysis of the gravity and topography of the Lada Terra shows that it is also
likely to be a hotspot. These features represent different geologic settings. Imdr and Dione are
similar to classical terrestrial style hotspot, will a broad topographic rise and 1-3 major volcanoes.
Themis Regio is a corona-dominated rise. It has a dozen volcanoes and a similar number of coronae,
which are thought to be manifestations of small-scale plumes. Many of the volcanoes and coronae
appear to have recent volcanism. This signature is interpreted as a plume coming from the core
mantle boundary that gets trapped at the upper-lower mantle boundary, giving rise to multiple small-
scale thermal diapirs. Lada Terra is in a class of its own, with a broad topographic swell, with a
peripheral trough, rift system, and volcanism. The presence of active mantle plumes on Venus
indicates that there must be a thermal boundary layer at the core-mantle boundary, giving rise to
plumes. Taken together, these features provide a picture of the interior of Venus that includes a hot
thermal boundary layer at the core, a phase transition at the base of the upper mantle, a deformable
lithosphere, and a mantle that is heating up.
Abstract Nr. 47
Are terrestrial exoplanets Earth-like, Venus-like, or different ?
Christophe Sotin, Jet Propulsion Laboratory - Caltech
Since the discovery of the first exoplanet in the nineties, hundreds of candidates have been reported.
Among them, about a dozen are reported to have a density that compares with terrestrial planets,
which make them preferred targets for spectral determination of their atmospheres. Venus and Earth,
although very close in density, have evolved on very different pathways: different atmospheric
composition, lack of current plate tectonics on Venus, liquid water on the Earth’s surface. Venus
dynamics is in the so-called ‘stagnant lid regime’ whereas the Earth’s surface is fractured into several
plates which move relative to each other in relation with mantle convection. Parameters such as
surface temperature, size and atmospheric composition may influence the transition from one regime
to the other. Most of the exoplanets found so far may be closer to Venus characteristics than to Earth.
Searching for Earth-like planets where plate tectonics operates is a major endeavor in the field of
exoplanets. However, this study also suggests that some exoplanets may be remnant cores of giant
planets that migrated towards their star while losing their atmosphere by escape processes.
This work has been performed at the Jet Propulsion Laboratory, California Institute of Technology,
MONDAY, 10 JUNE ‐ PAGE 2under contract to NASA. Government sponsorship acknowledged.
Abstract Nr. 82
The influence of rheology and volatiles on the geology of Venus
Ghail, Richard, Imperial College London
Pyroclastic activity is apparently almost absent on Venus, perhaps indicating a lack of volatiles in the
interior. However, an unusual feature near Diana Chasma likely originated as a pyroclastic surge
deposit. Its radar characteristics are only subtly different to those of the average Venus surface,
meaning that similar deposits may exist elsewhere but not be recognised and the interior may be
volatile-rich. Volatiles induce an asthenosphere, which together with decoupling of the crust and
mantle caused by the elevated surface temperature, enables stagnant lid recycling below the crust.
Fits to global hypsography imply a recycling rate of 5·0 ± 0·5 km² a⁻¹ and the loss of ~90% of a
scaled Earth-like heat production rate. Lid recycling by both plume activity and convection is
consistent with a number of features, particularly the global network of chasmata, by generating
major melting at upwelling sites, an adjacent region of minor melting aiding lateral slip, and
downwelling above geoid lows. An age of ~15 Ma is inferred for the western Eistla Regio plume and
subcrustal slip rates between 13 and 100 mm a⁻¹ are determined from fits to topographic profiles
across the principal chasmata. While Venus appears to be in thermal equilibrium now, higher rates of
radiogenic heat production in the past imply a greatly enhanced rate of magmatic resurfacing, which
1 Ga ago was capable of resurfacing the whole planet in ~40 Ma, implying a transition from an Io-like
volcanic planet to a tectonic dominated Earth-like regime over that time.
Abstract Nr. 05
Venus and Planetary Magnetism
Russell, Christopher T., UCLA; Cao, Hao, UCLA
A magnetic dynamo is a heat engine in which convection occurs in an electrically conducting medium.
As a planet cools rapidly, the transport of heat from the metallic core across the mantle to the surface
of the body does work by the production of a magnetic field. A source of heat from primordial thermal
energy (cooling of the core), radioactivity, latent heat release and expulsion of light fluids as a solid
inner core freezes all provide the necessary circulation and heat transport. In the case of a core in the
center of a planet, inefficient heat transport in the mantle and crust can stifle heat transport and shut
off a dynamo. This appears to have occurred on Venus. We review the physics of planetary dynamos
and Venus in particular. We also review the observational evidence on the current state of the Venus
dynamo.
Abstract Nr. 114
Large-scale magnetic flux ropes in low-altitude ionosphere of Venus: planetary origin or
solar wind origin
Luhmann, Janet G., UC Berkeley; Wei, Hanying, UCLA; Russell, Christopher T., UCLA; Zhang,
Tielong, Austrian Academy of Sciences
The Venus Express magnetometer observed large-scale magnetic structures of hundreds of kilometers
in spatial size near two hundred kilometer altitudes. Although occurring occasionally, these structures
strongly magnetize the low ionosphere (up to a hundred nano-tesla) and are quite different from the
small-scale magnetic flux ropes which are generated by the Venus-solar wind interaction with much
more frequent occurrence. Zhang et al. (2012) analyzed six such events in 2009 and suggest they
have different generation mechanism from the small-scale flux ropes, possibly crustal magnetic
remanent or magnetic reconnections. To understand the origin of these large-scale flux ropes, we
examine the 2009 data and find they occurs in about 10% of all orbits with locations very close to the
Venus geographic north pole (within 0.1 Venus radii). The correlation of occurrence with location and
MONDAY, 10 JUNE ‐ PAGE 3the eastward component always being positive are consistent with the flux ropes having planetary
origin. However, the field component radial from the surface changes polarity from orbit to orbit and
does not agree with a crustal field picture. Moreover, the polarity and variation of the radial field are
controlled by the orientation of the draped solar wind magnetic field in the Venus magnetosheath,
suggesting the flux rope having solar wind origin. In this paper, we investigate these large-scale flux
ropes to understand their generation mechanism.
MONDAY, 10 JUNE ‐ PAGE 4Tuesday, 11 June
Abstract Nr. 49
Physics of Induced Magnetosphere
Tielong Zhang, Space Research Institute, Austrian Academy of Sciences, Graz, Austria
The term induced magnetosphere has been widely used by the recent Venus Express publications. For
a planet like Venus or Mars, which has no global intrinsic magnetic field but with atmosphere, an
induced magnetosphere is created by the solar wind interaction with the highly conducting ionosphere.
It consists of regions near the planet and its wake for which the magnetic pressure dominates all other
pressure contributions. The induced magnetosphere is therefore analogous to the magnetosphere of
an intrinsically magnetized planet, but occupies a smaller volume. In this talk, we review some of the
induced magnetosphere observations by Venus Express.
Abstract Nr. 08
Comparative Plasma Interactions and their Effects at Venus, Mars and Titan
Luhmann, J.G.; Wang, Y-C.;Ledvina, S.A., SSL, University of California, Berkeley; Ma, Yingjuan; Wei,
Hanying; Russell, C.T.,IGPP UCLA; Zhang, T-L., IWF, Graz; Barabash, S., IRF, Kiruna; Kallio, E.;
Jarvinen, R., FMI; Sillanpaa, I., SWRI; Westlake, J.,JHUAPL; Fang, X., LASP, University of Colorado
The 'weakly magnetized planets' Venus, Mars and Titan represent a sequence of increasingly complex
plasma interactions-with increasingly complex consequences. Venus is perhaps the best understood
because it is a case where the incident flow is supersonic and the relevant scalings allow fluid plus test
particle treatments of the system. The Mars case adds not only the complexity of the crustal magnetic
fields but also an increasing need to consider finite ion gyroradius effects. Titan presents some other
complications including the presence of a permanent external field component from the Saturn dipole
and subsonic interaction with a highly nonthermal external particle population. And Titan's atmosphere
is also greatly extended compared to its planetary counderparts. We take a look at what we have
learned about some of the similarities and contrasts, and consider still open issues of interest for
future investigations and comparative studies.
Abstract Nr. 108
How the near-Venus space affects the planet
Stas Barabash, Swedish Institute of Space Physics
The solar wind flowing around Venus affects the planet’s atmosphere and ionosphere via energy,
matter, and momentum transfer. The energy transfer causes the non-thermal escape of planetary
ions. The matter transfer results in the deposition of the solar wind hydrogen and helium into the
atmosphere. The momentum transfer causes atmospheric sputtering. There might even occur
processes involving the angular momentum transfer to the upper ionosphere. We review the most
recent observations of all these processes by the ASPERA-4 instrument onboard Venus Express
(Analyzer of Space Plasmas and Energetic Atoms) and compare them with two other terrestrial
planets, Mars and Earth. The overall conclusion is at the present time the induced magnetosphere of
Venus creates a strong magnetic barrier substantially reducing the influence of the near-Venus
environment on the planet.
Abstract Nr. 95
Ion escape from Venus
TUESDAY, 11 JUNE – PAGE 5Stenberg Gabriella, Swedish institute of space physics; Barabash Stas, Swedish institute of space
physics; Futaana Yoshifumi,Swedish institute of space physics
We use more than three years of data from the ASPERA-4 instrument onboard Venus Express to
estimate the net outflow of protons and heavy ions from Venus.
The ion escape appears to exclusively take place in the induced magnetotail region and no heavy ions
are present in the magnetosheath. Protons of solar wind origin are travelling around the planet and
penetrating the tail, resulting in a mix of planetary and solar wind protons inside the induced
magnetosphere boundary. The escape rates of ions inside the tail agree with results from recent
published studies, where other analysis methods have been used.
We also present average flux patterns in the near Venus space based on computed average
distribution functions.
We compare our results for Venus with a recent study of ion escape from Mars, where the same
analysis method has been applied to data from the ASPERA-3 instrument on Mars Express.
Abstract Nr. 70
Dependence of O+ escape rate from the Venusian upper atmosphere on IMF directions:
ASPERA-4 observations
Masunaga Kei, Swedish Institute of Space Physics, Kiruna, Sweden; Futaana Yoshifumi, Swedish
Institute of Space Physics, Kiruna, Sweden; Stenberg Gabriella, Swedish Institute of Space Physics,
Kiruna, Sweden; Barabash Stas, Swedish Institute of Space Physics, Kiruna, Sweden; Zhang
Tielong, Space Research Institute, Austrian Academy of Science, Graz, Austria; Fedorov
Andrei, Centre d’Etude Spatiale des Rayonnements, Toulouse, France; Okano Shoichi, Institute for
Astronomy, University of Hawaii, Pukalani, HI, USA; Terada Naoki, Department of Geophysics,
Graduate School of Science, Tohoku University, Sendai, Japan
We present the dependence of O+ escape flux rate on the upstream interplanetary magnetic field
(IMF) direction calculated from the data obtained from the Analyser of Space Plasma and Energetic
Atoms (ASPERA-4) instrument and the magnetometer (MAG) onboard Venus Express. The data in the
period between June 21, 2006 and May 31, 2010 is classified into two cases: the perpendicular IMF
case (167 events) and the parallel IMF case (82 events), where IMF is nearly perpendicular to the
solar wind velocity and nearly parallel to it. We average O+ fluxes observed in the nightside region and
statistically calculate the escape rate for each IMF case. The O+ escape rates of (5.8 ± 2.9) × 1024 s-
1
(perpendicular IMF case) and (4.9 ± 2.2) × 1024 s-1 (parallel IMF case) are obtained. Since these
values are not significantly different, we conclude that several acceleration mechanisms must balance
each other in order to keep the escape rate constant.
Abstract Nr. 109bis
Comparisons of Venus Express measurements with an MHD model of O+ ion flows:
Implications for atmosphere escape measurements
McEnulty, Tess, LASP, University of Colorado, Boulder; Yingjuan Ma, IGPP, University of California, Los
Angeles; Janet G. Luhmann, SSL, University of California, Berkeley; Demet Ulusen, Space
Technologies Research Institute, Ankara, Turkey; Imke de Pater, Department of Astronomy, University
of California, Berkeley; Andrei Fedorov, Institut de Recherche en Astrophysique et Planetologie,
Toulouse, France; David Brain, LASP, University of Colorado, Boulder
The Venus Express (VEX) Ion Mass Analyzer (IMA) detects low energy (< 100 eV) oxygen ions flowing
into the wake. Investigators have suggested that the majority of the O+ escape measured by the IMA
is in this low energy population. However, the spacecraft potential and relative velocity complicate
interpretation of these ions. Due to these complications, there is still an open question of whether or
not all of these low energy ions are actually escaping. Some of the measured ions may actually be
gravitationally bound, even out to ~1.5 Venus radii in the wake. To illustrate these complications in
interpreting these measured low energy ions, we compare VEX ion measurements in this region to
results from a magnetohydrodynamic model. The model simulations highlight how IMA measurements
TUESDAY, 11 JUNE – PAGE 6of O+ can be affected by the spacecraft relative velocity and potential. In addition, we simulate
multiple different orbit trajectories in the model and show how the O+ IMA measurements depends on
orbit geometry and interplanetary magnetic field direction. We then integrate O+ escape flux in the
wake region of the model along the VEX orbit to illustrate how non-escaping (gravitationally bound)
ions could affect estimates of total O+ escape.
Abstract Nr. 101
Solar Wind energy and momentum transfer - Effects on the Venus polar thermosphere
Lundin Rickard, Swedish Institute of Space Physics; Barabash, S., Swedish Institute of Space Physics;
Futaana, S., Swedish Institute of Space Physics; Holmstrom, M., Swedish Institute of Space Physics;
Perez-de-Tejada. H., UNAM, Mexico City, Mexico; Sauvaud, J-A., CESR/CNRS Toulouse, France
An analysis of the average ion flow properties in the Venus magnetosphere and plasma tail reveals the
existence of a large-scale flow vortex, i.e. solar wind H+ (SW H+) and ionospheric O+ curling right-
handed tailward (as viewed from the Sun. The vortex commences at dusk (-Y), driven by a transverse
(to the solar wind) aberration flow component. Dusk magnetosheath and ionospheric ions move
westward across the nightside into the dawn sector, from where the tailward and lateral flow merges
into a tailward-moving vortex. Analyzing the fluid dynamics of the SW H+ energy and momentum
(E&M) transfer to O+ at the terminator, we find that E&M balance (efficiency ≈1) is achieved in the
altitude range 1200 - 600 km. Below 600 km a combined Westward O+ and energetic neutral atom
(ENA) flow completely dominates the momentum flux, the average O+ and ENA flow going in the
direction of the Venus atmospheric superrotation.
An analysis of the solar wind H+ ionospheric O+ energy and momentum (E&M) transfer to the neutral
gas in the Venus thermosphere and upper atmosphere over the polar region, reveals that
external/solar wind, and the corresponding ionospheric ion forcing, may drastically affect the short
term wind pattern down to 150 km. For instance, we find that the average ionospheric O+ wind is
capable, via ion drag, to set a polar cap CO2 air mass at 150-200 km altitude in motion by 200 m/s in
less than 5 minutes. Below 150 km, E&M transfer downward to the upper atmosphere is expected due
to frictional forcing, although at a much slower pace.
Abstract Nr. 107
The plasma vortex in the Venusian plasma tail. Steady-state reconnection or fluid motion?
Fedorov Andrey, IRAP/UPS/CNRS, Toulouse, France; S. Barabash, IRF, Kiruna, Sweden; T.L.
Zhang, University of science and technology, Hefei, China; J.A. Sauvaud, IRAP/UPS/CNRS, Toulouse,
France
The plasma and magnetic field statistics, accumulated since 2006 by Venus Express Aspera-4 and
MAG data show:
1. The minimum of the magnetic fileld in the close Venusian wake
2. The planetward averaged ion flow observed in the same region.
The case study (Zhang, 2012, Nature) gives at least one evidence of the plasmoid-like event that can
be associated with a tail magnetic reconnection.
The present paper combines statistical and case studies to answer the question: if the observed
plasma vortex is caused by a pseudo-steady state reconnection, or it is a characteristic fluid motion.
Abstract Nr. 74
Cosmic ray ionization in the Venusian atmosphere from Monte Carlo modelling
Tom Nordheim, Mullard Space Science Laboratory, University College London; Lewis R. Dartnell, UCL
Institute for Origins, University College London; Andrew J. Coates, Mullard Space Science Laboratory,
University College London
The atmospheres of the terrestrial planets are constantly exposed to solar and galactic cosmic rays,
TUESDAY, 11 JUNE – PAGE 7the most energetic of which are capable of affecting deep atmospheric layers through nuclear and
electromagnetic particle cascades. The energy deposited by these interactions is thought to be an
important driver for atmospheric chemistry and may possibly affect cloud microphysics, and in regions
beneath the penetration of ultraviolet radiation, cosmic rays are the primary ionization agent. It is
therefore crucial to quantify the amount of energy deposited by cosmic rays in the atmosphere by
altitude, as this is required to estimate ionization and conductivity profiles.
Detailed studies have considered the propogation of cosmic rays in the atmospheres of Earth, Mars,
Titan and the Giant Planets. However, to date, only a few studies (Dubach et al, 1974; Borucki et al,
1982) have considered such interactions in the Venusian atmosphere, notably using Boltzmann
transport approximations. In this work we will present preliminary results of full Monte Carlo modelling
of solar and galactic ray cosmic ray primaries interacting with the Venusian atmosphere during solar
minimum and maximum conditions. In addition, the radiation dose during extreme events (e.g
Carrington Flare event) will be discussed.
Abstract Nr. 02
Ionospheric magnetic fields and currents at Mars and Venus
Dubinin E., Max-Planck-Institute for Solar System Research, Lindau, Germany
Mars Express and Venus Express spacecraft have provided us a wealth of in-situ observations of
characteristics of induced magnetospheres of Mars and Venus at low altitudes during solar minimum
conditions. At such conditions large-scale magnetic fields are observed deeply in the ionospheres
(magnetized ionospheres). The observations again raise a long-standing question about the origin of
these fields. The problem is intimately related to the issue of electric current system and their closure.
Analysis of ASPERA-3, ASPERA-4, MARSIS and MAG data reveals a lot of features which require a
more sophisticated view at the origin and the topology of the ionospheric magnetic fields. Differing
perspectives at this problem are widely discussed.
Abstract Nr. 122
Fine structure of the Venus current sheet
Vasko Ivan, Space Research Institute, Moscow; Zelenyi Lev, Space Research Institute, Moscow;
Artemyev Anton, Space Research Institute, Moscow; Petrukovich Anatolii, Space Research Institute,
Moscow; Zhang Tielong, IWF, Graz; Fedorov Andrei, CNRS, France; Malova Helmi, Space Research
Institute, Moscow; Popov Viktor, Space Research Institute, Moscow; Nakamura Rumi, IWF, Graz
One of the gaps in our knowledge of the Venus current sheet (CS) is the CS thickness. The reason is
that the CS is in motion during observations (flapping motion) and the velocity of the flapping motion
cannot be determined by the single-spacecraft mission. On the other hand one can say something
about the CS spatial scale by studying the fine structure of magnetic field profiles. We have used the
data of Venus Express mission to study the structure of the Venus CS near the planet based on the
statistics of 13 CS crossings observed during steady conditions in the solar wind in years 2006-2010.
We have found that observed magnetic field profiles can be separated into single-scale and double-
scale. Plasma data have shown that double-scale CSs are oxygen-dominated, while single-scale CSs
can be proton-dominated as well as oxygen dominated. The observed profiles can be adequately
described in the frame of thin anisotropic CS model. The model predicts that double-scale CSs appear
due to the trapped oxygen population, picked up from the ionosphere. In addition the model predicts
that the CS thickness is only several particle gyroradii.
Abstract Nr. 93
Ionospheric photoelectron observations at Venus
Coates Andrew, UCL-MSSL; Wellbrock Anne, UCL-MSSL; Frahm Rudy, SwRI; Winningham
David, SwRI; Barabash Stas, IRF; Lundin R, IRF
TUESDAY, 11 JUNE – PAGE 8The Venus ionosphere at the top of the planet’s thick atmosphere is sustained by photoionization. The
consequent photoelectrons may be identified by specific features in the energy spectrum at 20-30 eV.
The ASPERA-4 electron spectrometer has an energy resolution designed to identify the photoelectron
peaks. Photoelectrons are seen not only in their production region, the sunlit ionosphere, but also at
more distant locations in the Venus environment. Here, we present a summary of the work to date on
observations of photoelectrons at Venus, and their comparison with similar processes at Titan and
Mars, and we present further data on the distant photoelectrons at Venus.
Abstract Nr. 86
A survey of Hot Flow Anomalies at Venus
G.A. Collinson, Heliophysics Science Division, NASA Goddard Space Flight Center, USA; D.G.
Sibeck, Heliophysics Science Division, NASA Goddard Space Flight Center, USA; A. Masters, Institute
of Space and Astronomical Science, JAXA, Japan; N. Shane,Mullard Space Science Laboratory,
University College London, UK; T.L. Zhang, Austrian Academy of Sciences, Space Research Institute,
Gratz, Austria; A. Fedorov, Universite de Toulouse, UPS-OMP, IRAP, Toulouse, France; S.
Barabash, Swedish Institute of Space Physics, Kiruna, Sweden; A.J. Coates, Mullard Space Science
Laboratory, University College London, UK; T.E. Moore,Mullard Space Science Laboratory, University
College London, UK; J.A. Slavin, University of Michigan, Ann Arbor, Michigan, USA
We present the first survey of Hot Flow Anomalies (HFAs) at the bow shock of Venus, expanding on
our recent initial case study of a single event [Collinson et al., 2012]. HFAs are an explosive plasma
phenomena, through the interaction between an interplanetary current sheet and a planetary bow
shock, wherein a pocket of reflected solar wind plasma becomes heated and rapidly expands. We
show that the newly discovered Cytherean HFAs are very important at Venus because: (1) they are
common, occurring at a rate of ~2 per day; (2) They are very large when compared to the overall size
of the system (0.4-1.7 Rv or (~130% of the sub-solar bow shock distance); and (3) unlike at
magnetized planets, occur very close (1.5-3Rv) to the surface of the planet. Given that the large
fluctuations in pressure associated with an HFA drive large motions in the location of the Earth’s
magnetopause, HFAs have the potential to be extremely disruptive to the induced magnetosphere and
unprotected ionosphere of Venus. Thus we hypothesize that HFAs have a much more dominant role in
the dynamics of the induced magnetosphere of Venus relative to the magnetospheres of magnetized
planets.
Abstract Nr. 09
The Implications of the Observed Evolution of the Co-Orbiting Material in 2201 Oljato’s
Orbit Observed by PVO and VEX
Russell, Christopher T., UCLA; Lai, Hairong, UCLA; Delzanno, Gian Luca, LANL; Zhang,
Tielong, Austrian Academy of Sciences
The observation with PVO and VEX of the time-varying IFE rate in the “Oljato-sensitive” sector of
ecliptic longitudes provides an important window into how “meteor” streams evolve. The fact that
there was a broad region of increased IFE occurrence centered around Oljato suggests that material
was broken free from Oljato sometime before 1980. These newly produced “bolides” themselves
evolved over a period of about 20 years so that they were no longer producing collisions in 2012. This
suggests that a warning system for Earth could be developed by launching a set of perhaps a dozen
small magnetometer-equipped spacecraft that would have a 1-year orbit period, but would orbit the
Sun in a slightly elliptical orbit so the satellites would spend time inside and outside 1 AU, but remain
ahead of the Earth in its orbit a fixed offset to provide time for analysis and follow-up. When swarms
of IFEs are seen at longitudes of known near-1-AU crossing objects, radar and optical measurements
could be made along that body’s orbit when the Earth reached that longitude. When hazardous co-
orbiting material was located, a decision could be made as to whether it was necessary to destroy or
remove it and how to accomplish this. We note that we already have spacecraft at 1 AU around Earth
and displaced from Earth (STEREO A and B). These spacecraft could be used to test this concept
before deployment.
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