MAGNETIC FIELDS OF EXOPLANETS. FEATURES AND DETECTION UCM, 27th May 2014 Enrique Blanco Henríquez.

Slides:



Advertisements
Similar presentations
IWF Graz … 1 H. Lammer (1), M. L. Khodachenko (1), H. I. M. Lichtenegger (1), Yu. N. Kulikov (2), N. V. Erkaev (3), G. Wuchterl (4), P. Odert (5), M. Leitzinger.
Advertisements

Plasma-induced Sputtering & Heating of Titan’s Atmosphere R. E. Johnson & O.J. Tucker Goal Understand role of the plasma in the evolution of Titan’s atmosphere.
Chapter 10 Our Star A Closer Look at the Sun Our Goals for Learning Why does the Sun shine? What is the Sun’s structure?
Chapter 11: Our Star © 2015 Pearson Education, Inc.
Copyright © 2012 Pearson Education, Inc. Chapter 10 Our Star 1.
Planets and Solar System Science at Low Frequencies Philippe Zarka LESIA, CNRS-Observatoire de Paris France Towards a European.
ESS 7 Lecture 14 October 31, 2008 Magnetic Storms
The Sun - Our Star Sun’s diameter 100 times the Earth’s
1 Diagnostics of Solar Wind Processes Using the Total Perpendicular Pressure Lan Jian, C. T. Russell, and J. T. Gosling How does the magnetic structure.
Solar wind interaction with the comet Halley and Venus
Or A Comparison of the Magnetospheres between Jupiter and Earth.
Neutron Stars and Black Holes PHYS390: Astrophysics Professor Lee Carkner Lecture 18.
Stellar Magnetospheres Stan Owocki Bartol Research Institute University of Delaware Newark, Delaware USA Collaborators (Bartol/UDel) Rich Townsend Asif.
Mars Global Surveyor Magnetometer - PI: M. Acuna.
Processes in Protoplanetary Disks
THE SUN 1 million km wide ball of H, He undergoing nuclear fusion. Contains 99% of the mass in the whole solar system! Would hold 1.3 million earths!
Stellar Winds and Mass Loss Brian Baptista. Summary Observations of mass loss Mass loss parameters for different types of stars Winds colliding with the.
X-ray Universe 2011 The High-Energy Environment of Extrasolar Planets J. Schmitt Hamburger Sternwarte Internet:
International Colloquium and Workshop "Ganymede Lander: scientific goals and experiments"
Tuija I. Pulkkinen Finnish Meteorological Institute Helsinki, Finland
Physical analogies between solar chromosphere and earth’s ionosphere Hiroaki Isobe (Kyoto University) Acknowledgements: Y. Miyoshi, Y. Ogawa and participants.
ABSTRACT This work concerns with the analysis and modelling of possible magnetohydrodynamic response of plasma of the solar low atmosphere (upper chromosphere,
The Sun and the Heliosphere: some basic concepts…
The EUV impact on ionosphere: J.-E. Wahlund and M. Yamauchi Swedish Institute of Space Physics (IRF) ON3 Response of atmospheres and magnetospheres of.
Collisions and transport phenomena Collisions in partly and fully ionized plasmas Typical collision parameters Conductivity and transport coefficients.
Solar Energy p-p chain is source of Solar Energy Sun could last 1.
Space Weather from Coronal Holes and High Speed Streams M. Leila Mays (NASA/GSFC and CUA) SW REDISW REDI 2014 June 2-13.
Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Helmut O. Rucker Exploring the Planets and Moons in our Solar System.
Terrestrial atmospheres. Overview Most of the planets, and three large moons (Io, Titan and Triton), have atmospheres Mars Very thin Mostly CO 2 Some.
Solar Wind and Coronal Mass Ejections
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Heliosphere: The Solar Wind March 01, 2012.
The Sun.
Space Science MO&DA Programs - September Page 1 SS It is known that the aurora is created by intense electron beams which impact the upper atmosphere.
A Transitional Fossil 375 Ma fish: flat nose, beginnings of limbs “Missing link” between fish and life on land.
Radio Astronomy Emission Mechanisms. NRAO/AUI/NSF3 Omega nebula.
© 2010 Pearson Education, Inc. 1. The Sun appears bright orange because of the extremely hot fires that are constantly burning carbon. TRUE or FALSE 2.
A generic description of planetary aurora J. De Keyser, R. Maggiolo, and L. Maes Belgian Institute for Space Aeronomy, Brussels, Belgium
Österreichische Akademie der Wissenschaften (ÖAW) / Institut für Weltraumforschung (IWF), Graz, Austria, iwf.oeaw.ac.atDownload:2014.
Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Chapter 10 Our Star.
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 10 Our Star A Closer Look at the Sun Our goals for learning: Why does the Sun shine? What is the Sun’s structure?
PARTICLES IN THE MAGNETOSPHERE
Jupiter and the Jovian Planets. Formation of Jovian Planets Step 1  Accretion of planetesimals to form large Earth-like solid planet cores of rocks,
Astronomy 1010 Planetary Astronomy Fall_2015 Day-35.
Atmosphere: Jupiter’s atmosphere has two basic features. 1) Changing parallel bands aligned with the equator, and 2) the Great Red Spot.
Satellites and interactions
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.
Shock heating by Fast/Slow MHD waves along plasma loops
The effects of the solar wind on Saturn’s space environment
Universe Tenth Edition Chapter 16 Our Star, the Sun Roger Freedman Robert Geller William Kaufmann III.
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Sun: Magnetic Structure Feb. 16, 2012.
The Sun. Properties M = 2 X kg = 300,000 M Earth R = 700,000 km > 100 R Earth 70% H, 28% He T = 5800 K surface, 15,000,000 K core.
The Gas Giants. JupiterSaturnUranusNeptune Mass (M Earth ) Distance from Sun (AU) Equatorial Radius (R Earth )
ASEN 5335 Aerospace Environments -- Magnetospheres 1 As the magnetized solar wind flows past the Earth, the plasma interacts with Earth’s magnetic field.
Aeronomy of extrasolar giant planets Tommi Koskinen (APL) APEX Meeting, Thursday 26th October 2006 HD b (an artist’s impression), © ESA 2004 (A.Vidal-Madjar)
Introduction to Plasma Physics and Plasma-based Acceleration
The Sun The SUN Chapter 29 Chapter 29.
GOAL: To understand the physics of active region decay, and the Quiet Sun network APPROACH: Use physics-based numerical models to simulate the dynamic.
Laser target interactions, and space/solar physics simulation experiments (Seed funding project) Laser-target: Boris Breizman, Alex Arefiev, Mykhailo Formyts'kyi.
Terrestrial atmospheres. Review: Physical Structure Use the equation of hydrostatic equilibrium to determine how the pressure and density change with.
Atmosphere: Jupiter’s atmosphere has two basic features
ESS 154/200C Lecture 16 Planetary Magnetospheres
Introduction to Space Weather Interplanetary Transients
GOAL: To understand the physics of active region decay, and the Quiet Sun network APPROACH: Use physics-based numerical models to simulate the dynamic.
ESS 154/200C Lecture 19 Waves in Plasmas 2
Introduction to Space Weather
Earth’s Ionosphere Lecture 13
Energy conversion boundaries
The Centre of the Solar System Earth Science 11
Presentation transcript:

MAGNETIC FIELDS OF EXOPLANETS. FEATURES AND DETECTION UCM, 27th May 2014 Enrique Blanco Henríquez

OUTLINE Magnetospheres of Earth-like exoplanets Dynamo mechanism Hot Jupiters magnetospheres Atmospheric escape from Hot Jupiters Magnetodisks Radio emission related to magnetic fields far-UV transits Bow-shocks

Magnetospheres in Earth-like exoplanets Magnetic field sustained by a dynamo mechanism In spite of major differences in structure, composition, and history, most of these dynamos are thought to be maintained by similar mechanisms: thermal and compositional convection in electrically conducting fluids in the planet interiors Tarter et al and Scalo et al recommended M-dwarfs as best targets to search for exo-Earths. M-dwarfs more active than Sun-like stars planets will be exposed to denser winds. However, Planets are tidally locked, are in synchronous rotation and have weak magnetic moments (maybe not as weak as we thought) Early model attempts Olson & Christensen (2006), independent of rotation rate

Magnetospheres in Earth-like exoplanets Nowadays, it is not know if F and D change with time However, rotation rate can play an important role in the nature of the magnetic field - Fast rotators dipole - Slow rotators multipole

Magnetospheres in Earth-like exoplanets Magnetic moment depends on its rotation rate, but also on it’s chemical composition and the efficiency of convection in its interior (F) Ω only marks if the dynamo is dipolar or multipolar, but magnetic moment strength will not explicitly depend on rotation. Planets under extreme conditions, i.e. highly inhomogeneous heating or under very strong stellar winds, may have their magnetic field affected. This is still work in progress and a better understanding of the interior structure and energy transportation mechanisms in rocky planets is still necessary.

Hot Jupiters Magnetospheres usual Giants Super-Earths Hot Jupiters

Hot Jupiters Magnetospheres Upper atmospheres subjected to intense heating and tidal forces Magnetic pressure dominates gas pressure (gas rarified) High temperatures generated by EUV heating Soft X-ray and EUV induced expansion of the upper atmosphere Thermal escape: Jeans escape – particles from tails Hydrodynamic escape – all particles Non-thermal escape: Ion pick-up Sputtering Photo-chemical energizing & escape Electromagnetic ion acceleration

Hot Jupiters Magnetospheres- importance of magnetodisk Huge amount of Hot Jupiters are efficiently protected against extreme plasma and radiation conditions. All estimations were based on too simplified model. It was considered a planetary dipole dominated magnetosphere only Dipole magnetic field balances stellar wind ram pressure However, big M is needed for efficient protection: big tidal locking small M Specifically for close-in exoplanets, new model is required Strong mass loss of a planet should lead to formation of a plasma disk A magnetodisk domaining magnetosphere More complete planetary magnetosphere model, including the whole complex of the magnetospheric electric current systems

Hot Jupiters Magnetospheres- importance of magnetodisk Formation of magnetodisk for Hot Jupiters “Sling” model: Dipole magnetic field drives plasma in co-rotation regimen inside the Alfvenic surface. “material-escape driven” models Hydrodynamic escape of plasma. Dipolar magnetic field provoques a charge separation which causes an electric field Hall current in equator plane.

Hot Jupiters Magnetospheres- importance of magnetodisk Paraboloid Magnetospheirc Model (PMM) for Hot Jupiters Key assumption: magnetopause is approximated by paraboloid of revolution along planet-star line -Planetary magnetic dipole -Magnetotail -Magnetodisk -Magnetopause currents -Magnetic field of stellar wind

Radio emission from exoplanets Interaction between the stellar wind and the magnetised planet provoques a reconnection that releases energetic electrons: radio emission Detection of cyclotron radio emission (CRE) would prove that the exoplanet is magnetised Electron cyclotron emission frequency : Radio Bode’s Law The radio flux observed at the Earth

Radio emission from exoplanets Optimal dynamos in the cores of terrestrial exoplanets: Magnetic field generation and detectability. Driscoll and Olson CRE for 32% and 65% CMF exoplanets - The ionospheric cutoff at 10 MHz sets the lower frequency limit for ground-based radio telescopes such as LOFAR. -LOFAR (LOw Frequency ARray) -It’s is possible to detect CRE? -Small fluxes -To be detectable with LOFAR, emission power must increase by a 1e3 factor

Measuring planetary magnetic field with transition observations Asymmetry between the ingress and egress times can be observed in the near- UV light curve compared to the optical observations (eg. WASP-12b) Led to suggest the existance of a bow-shock surrounding the planet’s atmosphere. For a shock to develop, the relative velocity between the planet and the stellar corona must be greater than local sound speed For a shock to be detected, it must compress the local plasma to a density high enough. For a hydrostatic, isothermal corona, the local density is Suppose that coronal material from the star is not magnetically confined, so it can escape in the form of a wind

Monte Carlo simulations for WASP-12b (early ingress) Measuring planetary magnetic field with transition observations

Measuring the planetary magnetic field (Vidotto et al. 2010) Measuring planetary magnetic field with transition observations