Energy conversion boundaries

Slides:



Advertisements
Similar presentations
Introduction to the Ionosphere
Advertisements

Review Vocabulary magnetic field: the portion of space near a magnetic or current-carrying body where magnetic forces can be detected The Sun contains.
Conceptual Model of the Earth’s Global Electric Field.
O. M. Shalabiea Department of Physics, Northern Borders University, KSA.
Reinisch_ Solar Terrestrial Relations (Cravens, Physics of Solar Systems Plasmas, Cambridge U.P.) Lecture 1- Space Environment –Matter in.
Crustal Fields in the Solar Wind: Implications for Atmospheric Escape Dave Brain LASP University of Colorado July 24, 2003.
11.1 Magnetic Dipole Field Magnetic Dipole Field (2) B 
9. Ionization and Energy Exchange Processes 1.Solar extreme ultraviolet (EUV) is the major source of energy input into the thermospheres/ionospheres in.
Julie A. Feldt CEDAR-GEM workshop June 26 th, 2011.
the Ionosphere as a Plasma
Physical analogies between solar chromosphere and earth’s ionosphere Hiroaki Isobe (Kyoto University) Acknowledgements: Y. Miyoshi, Y. Ogawa and participants.
The Atmosphere Chapter 17.1
The Sun. Sun Considered a medium STAR 93,000,000 miles away from Earth 1.39 million kilometers in diameter (one million Earths can fit inside the sun.
Sponge: List the six layers of the Earth.. Atmosphere A mixture of gases: N 2 78% O 2 21% Ar0.9% CO %
The EUV impact on ionosphere: J.-E. Wahlund and M. Yamauchi Swedish Institute of Space Physics (IRF) ON3 Response of atmospheres and magnetospheres of.
ESS 7 Lectures 15 and 16 November 3 and 5, 2008 The Atmosphere and Ionosphere.
Collisions and transport phenomena Collisions in partly and fully ionized plasmas Typical collision parameters Conductivity and transport coefficients.
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.
What is the Sun like? Chapter The Sun is the largest object in the solar system The Sun is the largest object in the solar system It’s diameter.
Magnetosphere-Ionosphere coupling processes reflected in
High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.
Composition of the Atmosphere. Carbon Dioxide Water Vapor 0-4% by volumn Variable Components of the atmosphere.
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © Ionosphere II: Radio Waves April 12, 2012.
Ionospheric Current and Aurora CSI 662 / ASTR 769 Lect. 12 Spring 2007 April 24, 2007 References: Prolss: Chap , P (main) Tascione: Chap.
The Sun Diameter – 865,000 miles Color – Yellow Star – Yellow Dwarf Mass – Earth = 1, Sun = 332,000 Surface Temperature – 12,000 degrees Fahrenheit (Hot.
CHAPTER 17 HEAT AND THE ATMOSPHERE HEATING THE ATMOSPHERE ENERGY FOR METEOROLOGY ORIGINATES IN THE SUN EARTH RECIEVES ONE 2 BILLIONTH OF SUNS ENERGY.
PHYS 1621 Proton-proton cycle 3 steps. PHYS 1622 Layers of the Sun Mostly Hydrogen with about 25% Helium. Small amounts of heavier elements Gas described.
Chapter 6 The Atmosphere Preview Section 1 Characteristics of the AtmosphereCharacteristics of the Atmosphere.
Response of the Earth’s environment to solar radiative forcing
1 MAVEN PFP ICDR May 23-25, 2011 Mars Atmosphere and Volatile EvolutioN (MAVEN) Mission Particles and Fields Science Critical Design Review May ,
Topics in Space Weather Earth Atmosphere & Ionosphere
PARTICLES IN THE MAGNETOSPHERE
Mass Transport: To the Plasma Sheet – and Beyond!
Reconstruction of Solar EUV Flux
ESS 200C Lecture 13 The Earth’s Ionosphere
The Sun By: JGilliam The Sun’s CompositionIdentifying Stars Composition ▪ Hydrogen and Helium together make up 99% of the sun’s mass. ▪ 75% of the sun’s.
Image credit: NASA Response of the Earth’s environment to solar radiative forcing Ingrid Cnossen British Antarctic Survey.
M. Yamauchi 1, H. Lammer 2, J.-E. Wahlund 3 1. Swedish Institute of Space Physics (IRF), Kiruna, Sweden 2. Space Research Institute (IWF), Graz, Austria.
1 Reconstruction of Solar EUV Flux Leif Svalgaard Stanford University EGU, Vienna, April 2015.
© Research Section for Plasma and Space Physics UNIVERSITY OF OSLO Daytime Aurora Jøran Moen.
Substorms: Ionospheric Manifestation of Magnetospheric Disturbances P. Song, V. M. Vasyliūnas, and J. Tu University of Massachusetts Lowell Substorms:
24 January, 20011st NOZOMI_MEX Science Workshop, Jan, 2001 R. Lundin, M. Yamauchi, and H. Borg, Swedish Institute of Space Physics H. Hayakawa, M.
ASEN 5335 Aerospace Environments -- Magnetospheres 1 As the magnetized solar wind flows past the Earth, the plasma interacts with Earth’s magnetic field.
Sponge: List the six layers of the Earth.
Plasma populations in the tail of induced magnetosphere
CEDAR Frontiers: Daytime Optical Aeronomy Duggirala Pallamraju and Supriya Chakrabarti Center for Space Physics, Boston University &
The Ionosphere and Thermosphere GEM 2013 Student Tutorial
Topic: Layers of the Atmosphere
The Atmosphere.
Mass-loading effect in the exterior cusp and plasma mantle
The Magnetosphere Feifei Jiang, UCLA
Upper Atmosphere Basics - I Neutral Atmosphere Vertical Structure
Shyama Narendranath Space Astronomy Group ISRO Satellite Centre
The Atmosphere Copyright © Houghton Mifflin Harcourt Publishing Company.
Ionosphere, Magnetosphere and Thermosphere Anthea Coster
Planetary Discovery in the era of Spacecraft Exploration Xi Zhang
Solar Interior.
Introduction to Space Weather
Reconstruction of Solar EUV Flux
Guided Notes about the Sun
Structure of the Atmosphere
Earth’s Ionosphere Lecture 13
Ionosphere References: Prolss: Chap. 4, P (main)
Main Idea: Energy is transferred throughout earths atmosphere
Introduction to Space Weather
The Centre of the Solar System Earth Science 11
The Ionosphere Equatorial Anomaly.
The Layered Atmosphere:
Layers of the Atmosphere
Magnetosphere: Structure and Properties
Presentation transcript:

Energy conversion boundaries

neutrals and ions

Ionospheric Layers

Ionospheric Layers Effective dynamo ~ dayside E-layer E: dynamo (only electrons can move freely due to i-n collision)  EM energy to Joule heating & geomagnetic induction F: highest density (highest energy absorption of solar EUV) but i-n collision is not sufficient  important for ion escape D: lowest layer of EUV heating (below is mesosphere with low-temperature)  mixing to non-mixing

Electron Density due to EUV < 102.7 nm The conductivity at a given height is proportional to the electron number density Ne. In the dynamo region the ionospheric plasma is largely in photochemical equilibrium. The dominant plasma species is O+2, which is produced by photo ionization at a rate J (s−1) and lost through recombination with electrons. N = √(J α-1 cos(χ))

E-layer as energy conversion boundary

Solar-Quiet (Sq) day ionospheric current system @ E-layer . Morning Evening A current system in the ionosphere is created and maintained by solar EUV radiation The magnetic effect of this system was what George Graham discovered

 since semi-static energy balance determines location of layer, it is strongly affected by the other element such as precipitating particles.

irregularity by precipitation

irregularity by precipitation Ne Te Ti Vi 36 hour data (EISCAT)

Atmospheric surfaces

Mesopause: stratified structure to possible convection layer  UV absorption by O3 below Tropopause: highest boundary of convection  UV absorption by O3 above It is not composition or force balance but the form of energy conversion that determines the mesopause/tropopause  dynamics/convection can easily modify the boundary

spin-off: Chapman-Ferraro current

spin-off: Chapman-Ferraro current If the motor-dynamo transition is considered as ”boundary layer”, the cusp is the kind of boundary layer from dayside interaction to nightside interaction.  ion dynamic can modify the boundary location

deceleration makes a pair of J//  We don’t need acceleration part to produce a pair of charge

detecting motion of “boundary” cusp Newell et al., 2010, JGR

Mass-loading boundary Plasma mantle is the largest source of the field-aligned current  solar wind is decelerated there inside the magnetopause  we need deceleration mechanism: due to mixture of escaping ions! Due to 16 time heavier mass of O+ than H+. the mass-loading of 0.1 cm-3 O+ to 10 cm-3 magnetosheath flow results in about 14% (=16/116) loss of velocity.

Mass-loading boundary Therefore, the Earth’s plasma mantle can be considered as boundary from magnetospheric ion regime to solar wind ion regime, which is equivalent to mass-loading. To have plasma mantle “mass-loading” boundary layer, escaping ions is inevitable, and this could be the reason why we have not found the plasma mantle for the Martian “cusp”