WIDE FIELD IMAGING OF MERCURY’S TAIL 2nd Meeting of the International Mercury Watch (IMW) Group Observatoire de Paris Observatoire de Paris 5-6 May 2008.

Slides:

Advertisements

Similar presentations

The Solar System By Level Two.

Advertisements

Slide 1 Stellar Evolution M ~4 P R O T O S T A R M a i n S e q u e n c e D G I A N T Planetary Supernova Nebula W h i t e D w a r f B r o w n D w a r f.

Kepler’s laws.

1/03/09 De 89 à 98. 1/03/09 De 89 à 98 1/03/09 De 89 à 98.

1 5 – 6 May 2008 IMW MeetingPARIS Observations (new) and Comparison with one (ours) Exospheric Model F. Leblanc Service d'Aéronomie du CNRS/IPSL.

Observational Constraints on the Interplanetary Hydrogen (IPH) Flow and the Hydrogen Wall John T. Clarke Boston University Boston University NESSC meeting.

Plate tectonics Image from

EXPERIMENTAL SETUP FOR BOSTON UNIV. MERCURY OBSERVATIONS FROM HALEAKELA.

AEOS Telescope + Image-Slicer/ Spectrograph Data Reduction and Results for June 8, 2006.

Observatoire de Paris, Paris, France May INTERNATIONAL MERCURY WATCH.

45 th ICFA Beam Dynamic Workshop June 8–12, 2009, Cornell University, Ithaca New York ECLOUD Simulations for the Tune Shift Measurements of December.

January 2012 Monday Tuesday Wednesday Thursday Friday Sat/ Sun / /8 14/15 21/22 28/

Plan for the next Mercury observation in Tohoku University M. Kagitani 1, Hirohito Fukazawa 1, S. Okano 1 1 Planetary Plasma and Atmospheric Research Center,

MERCURY OBSERVATIONS -- JUNE 2006 DATA REVIEW MEETING November 2006 Center for Space Physics, Boston University, College of Arts and Sciences.

Nov Boston Meeting1 Mercury at the TNG Cesare Barbieri Dept. of Astronomy University of Padova With the collaboration.

Mercury Data Review Tohoku Observatory Observation S. Okano 1, M. Kagitani 1, S. Kameda 2 1 Planetary Plasma and Atmospheric Research Center, Tohoku University.

First direct image of extrasolar planets billion miles.

Next week is the last section! Homework 6 is due next week in section Planet Walk “Extra credit” assignment is due by 12:10 next Friday (Slope Day) – but.

Using HMI to Understand Flux Cancellation by Brian Welsch 1, George Fisher 1, Yan Li 1, and Xudong Sun 2 1 Space Sciences Lab, UC-Berkeley, 2 Stanford.

Magnetospheric Morphology Prepared by Prajwal Kulkarni and Naoshin Haque Stanford University, Stanford, CA IHY Workshop on Advancing VLF through the Global.

Motion Field and Optical Flow. Outline Motion Field and Optical Flow Definition, Example, Relation Optical Flow Constraint Equation Assumptions & Derivation,

Mercury’s Sodium Tail McDonald Observatory “Narrow Field”

1 Synthesis Imaging Workshop Error recognition R. D. Ekers Narrabri, 14 May 2003.

NEW INSTRUMENTS AND TECHNIQUES 2nd Meeting of the International Mercury Watch (IMW) Group Observatoire de Paris Observatoire de Paris 5-6 May

Last time Martin Crow Crayford Manor House Astronomical Society About the use of binoculars. Types of mount. Telescope types. Finders, eye pieces, etc.

Comets and the Solar System Practical Astronomy: 16 September 2014 Tonight's Topics Planets over the next few months Three good comets are visible NOW!

Chapter 8, Astronomy. Identify planets by observing their movement against background stars. Explain that the solar system consists of many bodies held.

Plan for this week The jovian planets 5 major moons Comets, asteroids, and Earth impacts.

What stellar properties can be learnt from planetary transits Adriana Válio Roque da Silva CRAAM/Mackenzie.

THE SOLAR SYSTEM. By Nicholas and Dylan. The Solar System.

Optical Aeronomy Calibration Facility CEDAR WORKSHOP JUNE, 2007 Jeff Baumgardner, Center for Space Physics Boston University.

The Nature of Galaxies Chapter 17. Other Galaxies External to Milky Way –established by Edwin Hubble –used Cepheid variables to measure distance M31 (Andromeda.

Worlds around Distant Suns Mini University June 16, 2003 Among the most significant discoveries of the 20th Century.

The Solar System & Beyond Chapter 21. The Sun The closest star Center of our universe Made up of hydrogen and helium atoms that produce light and heat.

January 2nd 2013 Objective Warm-Up

December 7, 1631December 9, 1874 December 4, 1639December 6, 1882 June 6, 1761June 8, 2004 June 3, 1769June 6, 2012 Transits of Venus across the disk of.

Spatial Distribution of Atom Velocities in the Mercury Sodium Tail - Observation at Haleakala in June H. Fukazawa, M. Kagitani, S. Okano H. Fukazawa,

OBSERVING THE SUN & PLANETARY TRANSITS Petr HEINZEL Solar Physics Department Astronomical Institute of the Academy of Sciences Czech Republic.

Graduate student presentation: Subtracting the sky light International Mercury Watch Meeting Student: Cesare Grava Supervisor: Cesare Barbieri (Università.

Harry Kroto image at:

Multi-wavelength analysis of the impact polarization of 2001, June 15 th solar flare Zhi XU (1), Jean-Claude HENOUX (2), and Cheng FANG (3) (1) Yunnan.

© 2006 Plano ISD, Plano, TX/Klein ISD Edwin Hubble Hubble was born in Marshfield, Missouri. He earned a law degree and worked as a lawyer.

Astronomy Unit 2 Telescopes Celestial Spheres/Constellations Apparent Motion of the Stars Motion of the Planets.

Clouds and the Greenhouse Effect. The global average temperature on Earth is about 15 o C which is 30 o C more than it should be!

Measurements of White-Light Images of Cometary Plasma as a Proxy for Solar Wind Speed J.M. Clover, M.M. Bisi, A. Buffington, B.V. Jackson, P.P. Hick Center.

Pulsed Flows Along a Cusp Structure Observed with SDO/AIA B. J. Thompson 1, P. Démoulin 2, C. H. Mandrini 3, M. L. Mays 1, L. Ofman 4, S. L. Savage 1,

Characteristics of Stars. What is a galaxy? It is a cluster of stars (hundreds of billions of stars) It is a cluster of stars (hundreds of billions of.

Observation vs. Inferences The Local Environment.

Other planetary systems Are there other “solar systems” out there?

Planetary Radio Astronomy Bryan Butler. What kinds of things do we observe with the VLA? 45% - Extragalactic 20% - Galactic 30% - Stellar 5% - Solar system.

The formation of the solar system.. The Planets in Our Solar System Planet Distance from the Sun (Astrono mical Units miles km) Period of Revolut ion.

。 33 投资环境 3 开阔视野提升竞争力。 3 嘉峪关市概况。 3 。 3 嘉峪关是一座新兴的工业旅游城市，因关得名，因企设市，是长城文化与丝路文化交汇点，是全国唯一一座以长城关隘命名的城市。嘉峪关关城位于祁连山、黑山之间。 1965 年建市，下辖雄关区、镜铁区、长城区，全市总面积 2935.

Date of download: 7/6/2016 Copyright © 2016 SPIE. All rights reserved. Block diagram of the proposed method for quantitatively evaluating the observation.

By: Tiffany Pecorella Mercury is the first planet from the sun and looks a lot like Earth’s moon.

The Search for Another Earth. Exoplanets and the Kepler Space Telescope An exoplanet or extrasolar planet is a planet that orbits a star other than the.

Rosetta’s first view of CG

MSE Radial Resolution with ‘Dirty’ Lens

Astronomy 101 Whats up there?.

SOLAR FLARE OPTICAL SPECTROPOLARIMETRY

كيــف تكتـب خطـة بحـث سيئـة ؟؟

الدكتـور/ عبدالناصـر محمـد عبدالحميـد

Goal: To learn about the Kepler Mission and the Transit Method

Today! From Earth’s Perspective: Celestial Motion: Stellar Motion

Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November ,ApJ, 622,1251 J. Lin, Y.-K. Ko, L. Sui, J. C. Raymond, G.

[CII] observations of the Ring nebula (NGC 6720)

1 - January - Sun Mon The Wed Thu Fri Sat

Chapter 29 Review Part 2.

Peering through Jupiter’s clouds with radio spectral imaging

Presentation transcript:

WIDE FIELD IMAGING OF MERCURY’S TAIL 2nd Meeting of the International Mercury Watch (IMW) Group Observatoire de Paris Observatoire de Paris 5-6 May May 2008 Jeff Baumgardner Center for Space Physics, Boston University

WIDE FIELD IMAGING OF MERCURY’S TAIL REDUCED DATA SETS:  MAY 30, JUNE 1,2,3, 2007  NOVEMBER 12, 14, 2007  JANUARY 15,16,17, 2008

WIDE FIELD IMAGING OF MERCURY’S TAIL PLANETARY CONFIGURATION FOR OBSERVATIONS IN MAY-JUNE 2007 VELOCITY RELATIVE TO SUN: 9.3 to 8.6 Km/sec

WIDE FIELD IMAGING OF MERCURY’S TAIL MAY 30, 2007 SODIUM DATA ~ 8 degrees

WIDE FIELD IMAGING OF MERCURY’S TAIL MAY 30 DIFFERENCE MOVIE TO SHOW CLOUDS ~ 8 Degrees

WIDE FIELD IMAGING OF MERCURY’S TAIL JUNE 1, 2007 SODIUM DATA

WIDE FIELD IMAGING OF MERCURY’S TAIL JUNE 1, 2007 DIFFERENCE MOVIE

WIDE FIELD IMAGING OF MERCURY’S TAIL JUNE 2, 2007 SODIUM DATA

WIDE FIELD IMAGING OF MERCURY’S TAIL JUNE 2, DIFFERENCE MOVIE

WIDE FIELD IMAGING OF MERCURY’S TAIL 2 IMAGE AVERAGE FROM MAY 30 WITH RINGS AND SOME OF THE GRADIENT REMOVED

WIDE FIELD IMAGING OF MERCURY’S TAIL MAY 30, 2007 TAIL BRIGHTNESS PROFILES

WIDE FIELD IMAGING OF MERCURY’S TAIL PLANETARY CONFIGURATION FOR OBSERVATIONS IN NOVEMBER 2007 VELOCITY RELATIVE TO SUN: ~9 Km/sec

WIDE FIELD IMAGING OF MERCURY’S TAIL NOVEMBER 12, 2007 SODIUM DATA

WIDE FIELD IMAGING OF MERCURY’S TAIL NOVEMBER 12 DIFFERENCE MOVIE

WIDE FIELD IMAGING OF MERCURY’S TAIL NOVEMBER 14 SODIUM DATA

WIDE FIELD IMAGING OF MERCURY’S TAIL NOVEMBER 14 DIFFERENCE MOVIE

WIDE FIELD IMAGING OF MERCURY’S TAIL NOVEMBER 12, 2007 WITH RINGS AND GRADIENT REMOVED

WIDE FIELD IMAGING OF MERCURY’S TAIL NOVEMBER 12, 2007 TAIL BRIGHTNESS PROFILES

WIDE FIELD IMAGING OF MERCURY’S TAIL NOV 2007 MAY 2007

WIDE FIELD IMAGING OF MERCURY’S TAIL PLANETARY CONFIGURATION FOR OBSERVATIONS ON JANUARY 15,2008 VELOCITY RELATIVE TO SUN: Km/sec

WIDE FIELD IMAGING OF MERCURY’S TAIL JANUARY 15, 2008 SODIUM DATA

WIDE FIELD IMAGING OF MERCURY’S TAIL JANUARY 15, 2008 SODIUM DATA

WIDE FIELD IMAGING OF MERCURY’S TAIL JANUARY 15, 2008 SHIFTED AND STRECHED NO SODIUM TAIL APPARENT