'Mass ejections' presentation slideshows

Part 2: Stars

Part 2: Stars. Monday, February 10 Reading: Chapter 6 [Ed. 9, 10, 11, 12] The nature of light: How we use spectra to measure the properties of stars Wednesday, February 12 Reading: Chapters 8, 9.1, 9.5 or Orion Nebula Stars: distance, luminosity, mass, composition. Star formation.

553 views • 41 slides

Space Research Institute Graz Austrian Academy of Sciences

Space Research Institute Graz Austrian Academy of Sciences. Exploring the Planets and Moons in our Solar System. Helmut O. Rucker. CERN, Geneve, June 2006. Space Research Institute Graz Austrian Academy of Sciences. Exploring the Planets and Moons in our Solar System.

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558 views • 30 slides

The Sun, our favorite star!

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A modest G2 star, conveniently located 150,000,000 km from Earth.

The Sun. A modest G2 star, conveniently located 150,000,000 km from Earth. Solar Interior. The core is the energy source, where hydrogen fuses into helium. Heat from the core spreads out through the radiative and convective zones. How do we know...?.

386 views • 27 slides

Satellite Missions and Observations

Satellite Missions and Observations. Dan Gershman SHINE Student Day 7/10/2011. This talk. Overview What makes each spacecraft dataset important? Where can you get all this data? Summary. Overview of current missions. http://science.nasa.gov/missions/.

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SolarFlows Dr. Gabriele Pierantoni (TCD)

SolarFlows Dr. Gabriele Pierantoni (TCD). Contents. What is Heliophysics ? How could workflows help ? Some examples What we are doing. Solar and Helio physics.

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Our Sun!

Our Sun!. Health Warning: Avoid Direct Eye Contact. How can we learn about something as hot as the Sun?. Humans have sent spacecraft up to study our star. The SOHO spacecraft has been in operation since 1996 .

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Milestones in commercial space weather: the USU Space Weather Center

Milestones in commercial space weather: the USU Space Weather Center. USU Innovation and Invention Awards Reception Thursday, 01 April 2010 W. Kent Tobiska, Director Herbert C. Carlson, Director Strategic Development USU USTAR Space Weather Center. USU Space Weather Center.

406 views • 18 slides

Instrumental & Technical Requirements

Instrumental & Technical Requirements. Science objectives for helioseismology. Understanding the interaction of the p -mode oscillations and the solar magnetic field + Resolving the discrepancies between local helioseismic methods = Accurate determination of structure below sunspots +

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High-cadence Radio Observations of an EIT Wave

High-cadence Radio Observations of an EIT Wave. S. M. White and B. J. Thompson 2005, ApJ, 620, L63. OKAMOTO Joten/Takenori (D1). Abstract. Radio observations of the 1997 September 24 EIT wave The radio spectrum is consistent with optically thin coronal emission.

294 views • 13 slides

STEREO

STEREO. By: Abby Bradshaw Paige Taylor. What is STEREO?.

237 views • 5 slides

Today:

Today:. Neutrinos Solar atmosphere: Photosphere granulation Chromosphere spicules Corona Solar wind Solar magnetic fields Sunpots Sunspot cycle Reconnection, flares, prominences and coronal mass ejections. Neutrinos. Solar atmosphere: photosphere.

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