Rafkin et al VTGCM1 VTGCM and Applications to VEX and PVO Data Analysis: Upgraded Simulations (F10.7 ~70 & 200) Venus Express Science Meeting Thuile, Italy.

Slides:



Advertisements
Similar presentations
INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 1 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department.
Advertisements

Basics & Motivation Technique & Observations Fits & Measurements Summary & Outlook Atmospheric Wave Workshop ESTEC 11/10/2011 Tobias Stangier I st Physics.
Zasova L.V., Shakun A.V., Khatuntsev I.V., Ignatiev N.I,(1,2), Brekhovskih U.A.(1), Piccioni G.(3), Drossart P.(4). (1) IKI RAS, Moscow, (2) MIPT, Dolgoprudny,
1 Ionospheres of the Terrestrial Planets Stan Solomon High Altitude Observatory National Center for Atmospheric Research
MURI,2008 Electric Field Variability and Impact on the Thermosphere Yue Deng 1,2, Astrid Maute 1, Arthur D. Richmond 1 and Ray G. Roble 1 1.HAO National.
The primary mechanism through which energy and momentum are transferred from the lower atmosphere to the upper atmosphere and ionosphere is through the.
Non-magnetic Planets Yingjuan Ma, Andrew Nagy, Gabor Toth, Igor Sololov, KC Hansen, Darren DeZeeuw, Dalal Najib, Chuanfei Dong, Steve Bougher SWMF User.
SBUV/2 Observations of Atmospheric Response to Solar Variations Matthew DeLand Science Systems and Applications, Inc. (SSAI) Background -SBUV/2 instruments.
ISSI Meeting, Bern January 2014 New 3D photochemical global model with ions in D-region: The instrument for solar-atmospheric relations study Alexei.
Oxygen: Stratosphere, Mesosphere and Thermosphere Part-3 Chemical Rate Equations Ozone Density vs. Altitude Stratospheric Heating Thermal Conductivity.
Modeling the Distribution of H 2 O and HDO in the upper atmosphere of Venus Mao-Chang Liang Research Center for Environmental Changes, Academia Sinica.
Modeling the Distribution of H 2 O and HDO in the upper atmosphere of Venus Mao-Chang Liang Research Center for Environmental Changes, Academia Sinica.
Using global models and chemical observations to diagnose eddy diffusion.
The ionosphere of Mars and its importance for climate evolution A community white paper for the 2009 Planetary Decadal Survey Paul Withers
Research at Boston University on the upper atmosphere of Mars Paul Withers and Majd Matta MEX Workshop ESTEC, The Netherlands.
The Martian Upper Atmosphere By Paul Withers, newly graduated from LPL’s PhD program Dissertation on “Tides in the Martian Atmosphere” Lecture given to.
1 Two-Dimensional Chemistry Transport Model 11/16/2006.
The Response of an Ionosphere to changes in the solar F 10.7 flux: Comparison of Venus, Earth and Mars Paul Withers and Michael Mendillo Boston University.
Determination of upper atmospheric properties on Mars and other bodies using satellite drag/aerobraking measurements Paul Withers Boston University, USA.
November 2006 MERCURY OBSERVATIONS - JUNE 2006 DATA REVIEW MEETING Review of Physical Processes and Modeling Approaches "A summary of uncertain/debated.
The Martian Ionosphere in Regions of Crustal Magnetic Fields Paul Withers, Michael Mendillo, Dave Hinson DPS 2004, Louisville, Kentucky,
How do gravity waves determine the global distributions of winds, temperature, density and turbulence within a planetary atmosphere? What is the fundamental.
Rosetta_CD\PR\what_is_RS.ppt, :39AM, 1 Mars Express Radio Science Experiment MaRS MaRS Radio Science Data: Level 3 & 4 The retrieval S.Tellmann,
Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.
New Insights into the Atmospheric Chemistry of Venus from Venus Express Yuk L. Yung Caltech GISS Seminar, Mar
Exosphere Temperature Variability at Earth, Mars and Venus
Chemistry of Venus’ Atmosphere Vladimir A. Krasnopolsky Photochemical model for km Photochemical model for km Chemical kinetic model for.
*K. Ikeda (CCSR, Univ. of Tokyo) M. Yamamoto (RIAM, Kyushu Univ.)
Photochemical Control of the Distribution of Venusian Water and Comparison to Venus Express SOIR Observations Christopher D. Parkinson 1, Yuk L. Yung 2,
How does the Sun drive the dynamics of Earth’s thermosphere and ionosphere Wenbin Wang, Alan Burns, Liying Qian and Stan Solomon High Altitude Observatory.
Venus : the lost world Pierre Drossart LESIA, Observatoire de Paris.
1 Agenda Topic: Space Weather Modeling and the Whole Atmosphere Model (WAM) Presented By: Rodney Viereck(NWS/NCEP/SWPC) Contributors: Rashid Akmaev (SWPC)
Neutral Winds in the Upper Atmosphere Qian Wu National Center for Atmospheric Research.
Scott M. Bailey, LWS Workshop March 24, 2004 The Observed Response of the Lower Thermosphere to Solar Energetic Inputs Scott M. Bailey, Erica M. Rodgers,
The ionosphere of Mars never looked like this before Paul Withers Boston University Space Physics Group meeting, University of Michigan.
Observing Venus From a Balloon Platform Ohio Aerospace Institute Cleveland, Ohio.
1 The effects of solar flares on planetary ionospheres Paul Withers and Michael Mendillo Boston University 725 Commonwealth Avenue, Boston MA 02215, USA.
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © Ionosphere II: Radio Waves April 12, 2012.
GITM and Non-hydrostatic processes Yue Deng Department of Physics University of Texas, Arlington.
COMPARATIVE TEMPERATURE RETRIEVALS BASED ON VIRTIS/VEX AND PMV/VENERA-15 RADIATION MEASUREMENTS OVER THE NORTHERN HEMISPHERE OF VENUS R. Haus (1), G. Arnold.
Response of the Earth’s environment to solar radiative forcing
Abstract Dust storms are well known to strongly perturb the state of the lower atmosphere of Mars, yet few studies have investigated their impact on the.
Studying the Venus terminator thermal structure observed by SOIR/VEx with a 1D radiative transfer model A. Mahieux 1,2,3, J. T. Erwin 3, S. Chamberlain.
Image credit: NASA Response of the Earth’s environment to solar radiative forcing Ingrid Cnossen British Antarctic Survey.
1 Observations of tides and temperatures in the martian atmosphere by Mars Express SPICAM stellar occultations Paul Withers 1, Jean-Loup Bertaux 2, Franck.
Night OH in the Mesosphere of Venus and Earth Christopher Parkinson Dept. Atmospheric, Oceanic, and Space Sciences University of Michigan F. Mills, M.
STRUCTURE AND BEHAVIOR OF PLANET VENUS BY: ANTON ESCARIO upload.wikimedia.or g.
The ionosphere of Mars and its importance for climate evolution A community white paper for the 2009 Planetary Decadal Survey Paul Withers
How the ionosphere of Mars works Paul Withers Boston University Department Lecture Series, EAPS, MIT Wednesday :00-17:00.
Energy inputs from Magnetosphere to the Ionosphere/Thermosphere ASP research review Yue Deng April 12 nd, 2007.
Coupled Thermosphere Ionosphere Plasmasphere Model with self-consistent Electrodynamics (CTIPe) Global thermosphere km, solves momentum, energy,
Impact of midnight thermosphere dynamics on the equatorial ionospheric vertical drifts Tzu-Wei Fang 1,2 R. Akmaev 2, R. Stoneback 3, T. Fuller-Rowell 1,2,
When Lower Atmosphere Waves Invade the Upper Atmosphere
Using the Mars climate Database for aerobraking ( km)
VEx – Akatsuki co-ordinated observations
Atmosphere-Ionosphere Wave Coupling as Revealed in Swarm Plasma Densities and Drifts Jeffrey M. Forbes Department of Aerospace Engineering Sciences, University.
Welcome to Equatorial-PRIMO
GOMOS measurements of O3, NO2, and NO3 compared to model simulations
Thermosphere-Ionosphere Issues for DASI - I:
Tomoko Matsuo DAI/GSP *in collaboration with Jeff Anderson(DAI),
Astrid Maute, Art Richmond, Ben Foster
Earth’s Ionosphere Lecture 13
Ionosphere References: Prolss: Chap. 4, P (main)
Exploring the ionosphere of Mars
Exploring the ionosphere of Mars
Comparisons and simulations of same-day observations of the ionosphere of Mars by radio occultation experiments on Mars Global Surveyor and Mars Express.
The Upper Atmosphere: Problems in Developing Realistic Models
Variation of Protonated Ions and H2 as observed by MAVEN NGIMS
VarSITI Closing Simposium, Sofia, Bulgaria, June 2019
NASA’s Global-scale Observations of the Limb and Disk (GOLD) Mission: Unprecedented Imaging of the Boundary Between Earth and Space Richard Eastes GOLD.
Presentation transcript:

Rafkin et al VTGCM1 VTGCM and Applications to VEX and PVO Data Analysis: Upgraded Simulations (F10.7 ~70 & 200) Venus Express Science Meeting Thuile, Italy March 18-24, 2007 S. Bougher and A. Brecht (U. of Michigan) S. Rafkin and A. Stern (SwRI-Boulder) Contact: or This work was funded in part by the NASA Venus Express Participating Scientist Program under grant NNG06GC76G.

Rafkin et al VTGCM2 Upper Atmosphere Datasets at Venus  Pioneer Venus Orbiter ( ) -- F10.7 ~ 200 (in-situ at start) and 130 (entry at end) -- OUVS (airglow, neutral density and T structure) -- ONMS (neutral density and T structure) -- OETP (electron T and density) -- RPA (ion T and density)  Venus Express (June 2006 to date) -- F10.7 ~ (primary mission) -- SPICAV (airglow, neutral density and T structure) -- VeRA (radio occultation; T-structure; electron density profiles) -- VIRTIS (O 2 airglow, T structure, inferred winds) -- VMC (visible and IR camera, O 2 airglow)

Rafkin et al VTGCM3 Venus Atmosphere Regions and Processes

Rafkin et al VTGCM4 Venus Thermospheric General Circulation Model (VTGCM) Formulation and Structure  Altitude range: ~ km (day); km (night)  5x5º latitude-longitude grid (pole-to-pole)  Pressure vertical coordinate (1/2-H intervals): 34-levels  Major Fields: T, U, V, W, O, CO, N 2, CO 2, Z  PCE ions Fields: CO 2 +, O 2 +, N 2 +, NO+, O+, Ne  Minor Fields: O 2 (and O 2 IR nightglow at 1.27  m)  Future Minor Fields: N( 4 S), N( 2 D) (and NO nightglow)  Full 2-hemispheric capability. Timestep = 60.0 secs.  Venus obliquity ~ 177.4º (“seasonal” cases possible)  Rayleigh friction used to slow SS-AS winds.  Weak RSZ winds prescribed at model lower boundary  Upgraded airglow capability: O 2 -IR, NO-UV(future)

Rafkin et al VTGCM5 VTGCM Science Goals in Support of VEX  Compare the modeled structure of the atmosphere (up to 180 km) with high vertical resolution solar/stellar occultations, especially in middle to high latitudes;  Use observed spatial distributions of NO, O, and H airglows, at spatial resolutions substantially better than existing data, and interpret these global tracers of the thermospheric circulation with the VTGCM;  Determine the dynamical processes that link the Venus middle and upper atmospheres (tides, planetary, and gravity waves, etc.) through general circulation modeling of the thermosphere;  Compare and contrast the response of the Venus atmosphere with that of Mars—where the sister spacecraft (Mars Express) and SPICAM is in orbit, and where the Mars Reconnaissance Oribiter was simultaneously aerobraking in 2006—under the same solar cycle forcing.

Rafkin et al VTGCM6 Input Parameters for VTGCM Simulations: VEX & PVO  F10.7 ~ 70, 130, 200. Solomon UV routine ( nm).  Factor for heliocentric distance = Equinox (only).  Q-Efficiency (EUV, UV) = 20, 22% (after Fox, 1988)  Slant column integration for Chapman functions.  K(O-CO 2 ) = 3.0 x cm 3 /sec at 300K  CO  m cooling scheme from Bougher et al., (1986).  K zz ≤ x10 7 cm 2 /sec. Prandtl # = 10.0  Fox & Sung (2001) ion-neutral chemical reactions & rates.  O & CO sources and losses explicitly calculated.  Te from Theis and Brace (1993). Ti = Tn.  No Venus rotation. Static (GM) LBC (densities and T)

Rafkin et al VTGCM7 T+(U,V) at Exobase VEXPVO U<185 m/sT<230KU<220 m/sT<300K

Rafkin et al VTGCM8 Temperature (K) at Equator VEXPVO T(DY)<230KT(NT)>100KT(DY)<300KT(NT)>100K

Rafkin et al VTGCM9 Solar Cycle T exo & T 140 Variations (LAT = 2.5N; SLT = 1200) T 140 ~ 200 to 240K F10.7 ~ 70 to 240 units * PVO * MGN Texo ~ 230 to 325K F10.7 ~ 70 to 240 units ΔTexo ~ 95 K *VEX?

Rafkin et al VTGCM10 U and W at Equator VEXPVO U (m/s) W (s -1 ) (Multiply By SHT for m/s) Min: m/s Max: 0.25 m/s Min: -186 m/s Max: 173 m/s Min: -220 m/s Max: 200 m/s Min: -0.6 m/s Max: 0.45 m/s

Rafkin et al VTGCM11 Concentration (#/cm 3 ) at Equator Nightside Peak: 6.0x10 11 cm -3 Nightside Peak: 7.9x10 11 cm -3 Nightside Peak: 6.7x10 12 cm -3 Nightside Peak: 7.7x10 12 cm -3 VEX PVO log10[O]log10[CO]log10[CO 2 ]

Rafkin et al VTGCM12 Electron Density (#/cm 3 ) at Equator (VEX): log10[Ne] [Ne] < 4.0x 10 5 Peak [Ne] ~138 km.

Rafkin et al VTGCM13 Peak Electron Density Variations (LAT = 2.5N; SLT = 12; ALT ~ 140 km) SMIN = 4.1 x 10 5 cm 3 /sec SMAX = 7.0 x 10 5 cm 3 /sec * PVO * Venera 9-10 *VEX?

Rafkin et al VTGCM14 Molecular O 2 at Equator log10[O 2 ] #/cm 3 Molecular O 2 IR Nightglow at Equator (log10 (ph/cm 3/ sec) Peak V.E.R. of 7.7x10 5 ph/cm km. Peak Intensity: ~ MR

Rafkin et al VTGCM15 Summary and Conclusions  Upgraded VTGCM code is operational for 4-major and 1-minor species plus several photochemical ion species.  Production simulations over the solar cycle (and weak Venus seasons) are completed. Comparisons to PVO, Magellan drag (MGN), and VEX datasets are starting.  O 2 IR nightglow calculations are available for new comparisons to VEX datasets (when available).  Gravity wave breaking formulations will be soon incorporated into the VTGCM: (a) to provide self- consistent RSZ winds and needed momentum drag, and (b) to produce unique circulation patterns giving rise to variable O 2 and NO nightglow intensity distributions.