CDS Images at Different Spectral Lines - Temperatures

Slides:

Advertisements

Similar presentations

Solar Flares, CMEs, and Satellites, Oh My! M.M. Montgomery, PhD University of Central Florida LWS Heliophysics Summer School 2013.

Advertisements

The Sun 6.E.1.2 Explain why Earth sustains life while other planets do not based on their properties (including types of surface, atmosphere.

The Sun 6.E.1.2 Explain why Earth sustains life while other planets do not based on their properties (including types of surface, atmosphere.

Chapter 8 The Sun – Our Star.

The Solar Corona and Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics.

General Properties Absolute visual magnitude M V = 4.83 Central temperature = 15 million 0 K X = 0.73, Y = 0.25, Z = 0.02 Initial abundances: Age: ~ 4.52.

Space Weather Causes and Consequences An introduction to Space Weather What is it? Where does it come from? Who is impacted? Rodney Viereck NOAA Space.

1 Grades 3 - 5: Introduction. 2 Better Observation Of The Sun And Earth Importance of Space Technology.

Space Weather How fast does solar activity affect Earth?

7 THE SUN The star we see by day. 7 Goals Summarize the overall properties of the Sun. What are the different parts of the Sun? Where does the light we.

Chapter 7 The Sun. Solar Prominence – photo by SOHO spacecraft from the Astronomy Picture of the Day site link.

Solar system science using X-Rays Magnetosheath dynamics Shock – shock interactions Auroral X-ray emissions Solar X-rays Comets Other planets Not discussed.

Stephanie Moats Mentor: Kathy Reeves August 2009 Harvard-Smithsonian Center for Astrophysics.

Solar Rotation Lab 3. Differential Rotation The sun lacks a fixed rotation rate Since it is composed of a gaseous plasma, the rate of rotation is fastest.

Announcements Observing Monday-Thursday of this week counts on the third exam. Fourth exam is Wednesday, November 17 Review will be Monday, November 15.

Space Weather Major sources of space weather ● Solar wind – a stream of plasma consisting of high energy charged particles released from the upper atmosphere.

Grade 9 Academic Science.  the center of our solar system – heliocentric model.  the Sun has many different layers – each performing different activities.

The Sun Our Nearest Star. The Source of the Sun’s Energy The Source of the Sun’s Energy Fusion of light elements into heavier elements. Hydrogen converts.

Chapter 20, Section 2 The Sun Anne Marie Scrudato’s notes borrowed by Rusty Sturken.

For Us, the sun is the provider of Energy; The Provider of Life.

Chapter 9 The Sun. 9.4 The Active Sun Sunspots: appear dark because slightly cooler than surroundings:

K9LA Vancouver 2003 Disturbances to Propagation Carl Luetzelschwab K9LA CQ DX?Where’d everybody go?

The Sun- Solar Activity. Damage to communications & power systems.

Stars Physics Astrophysics. Brightness Different brightness. Different color. How bright are they really? What is due to distance? What is due.

Solar Wind and Coronal Mass Ejections

The Solar Wind.

Sunspots. X-ray solar image Solar Flair Solar Corona.

SOLAR FLARES AND ERUPTIONS Lyndsay Fletcher University of Glasgow.

THE SUN. The Sun The sun has a diameter of 900,000 miles (>100 Earths could fit across it) >1 million Earths could fit inside it. The sun is composed.

Solar and STP science with AstroGrid Silvia Dalla School of Physics & Astronomy, University of Manchester A PPARC funded project.

Our Sun 93 million miles from Earth 150 million kilometers Earth 99.8% of the mass of our solar system.

Sunny Spells and Solar Storms: understanding space weather with LUCID.

Solar Astronomy Space Science Lab 2008 Pisgah Astronomical Research Institute.

The Sun. About three quarters of the Sun's mass consists of hydrogen, while the rest is mostly helium. The Sun, like most stars, is a main sequence star,

1 Grades 6-8: Introduction. 2 Aerospace Technology Space Science Human Exploration And Development Of Space Earth Science Main Areas Of Research.

Analysis of 3 and 8 April 2010 Coronal Mass Ejections and their Influence on the Earth Magnetic Field Marilena Mierla and SECCHI teams at ROB, USO and.

Agenda: Here comes the sun March 18 and 21 1.Learning Target: I can describe how sunspots are important 2.Agenda 1.Danger Solar Storm DVD and Questions.

 Electromagnetic Radiation › Gamma rays, X-rays, UV light, visible light, infrared radiation, microwaves, and radio waves › All energy travels through.

Detecting, forecasting and modeling of the 2002/04/17 halo CME Heliophysics Summer School 1.

The Sun A cool animation of the Sun can be found on this link, click and scan down. An animation.

THE SUN The star we see by day.

Sun: General Properties

The Sun – Our Star.

The Sun All images and information courtesy of SOHO consortium. SOHO is a project of international cooperation between ESA and NASA."

SLIDE SHOW 6. SOLAR WIND (Mariner 2, 1962)

California Standards: 1a, e.

Nuclear Fusion & Solar Activity

The Sun A cool animation of the Sun can be found on this link, click and scan down. An animation.

Solar Activity and Space Weather

The Sun: close-up of a spectral class G main sequence star

Solar and Heliospheric Physics

Chapter 29-2 Solar Activity.

Section 2: Solar Activity

Do Now 12/9/09 What is the sun made of???

High-cadence Radio Observations of an EIT Wave

SIDC Space Weather Briefing

SIDC Space Weather Briefing

Grades 3 - 5: Introduction

The Centre of the Solar System Earth Science 11

Grades 9-12: Introduction

SIDC Space Weather Briefing

SIDC Space Weather Briefing

Grades 3 - 5: Introduction

SIDC Space Weather Briefing

SIDC Space Weather Briefing

CORONAL MASS EJECTIONS

SIDC Space Weather Briefing

SIDC Space Weather Briefing

Presentation transcript:

CDS Images at Different Spectral Lines - Temperatures

Recent Scientific Advance: Detection of Supersonic Shock from Solar Flare Discovery of coronal shock wave running across the solar disk. Shock wave was generated by April 7, 1997 solar flare; also caused a large halo mass ejection. Left image is Fe XII at 195 A, formed at a temperature of about 1.5 million degrees. Shock is shown in black and white difference images where each image shows the difference from the previous image. The speed at which the blast wave moved across the solar disk was estimated at 400 km/sec - supersonic speed. Supersonic shock from solar flare

Comet (vs time)

ACE WIND POLAR

Sun-Earth Connection: Images of Solar Event and Terrestrial Response Solar flare, blast wave, and Coronal ‘Halo” Mass Ejection observed on April 7, 1997 by SOHO Radio emission from shockfront tracked from Sun to Earth by WIND • Aurorae observed in visible, UV, and X-rays by POLAR and from ground(e.g. Boston) April 11. Tempo 2 comsat loses 15% of power on April 11, attributed to solar event Event is lead story on Dan Rather’s Evening News Comet Hale-Bopp Photo: F. Sienkewicz

The Geomagnetic Storm of 11 April 1997: Global, Synoptic, Regional, and Local Effects NASA/POLAR CEPPAD/IPS ENA Imager Synoptic Auroral Intensification Viewed above Earth’s North Pole Global Van Allen Belt Enhancement as Viewed from Space NASA/POLAR PIXIE X-Ray Imager Boston University All-Sky Auroral Imaging System Regional Auroral Emissions Measured from Ground Imagers Photo courtesy of F. Sienkiewicz, Boston University Visible Aurora Seen Locally, North from Gloucester, MA HESpence, Boston University Center for Space Physics, 10/16/97

Solar Mass Ejection Imager (SMEI) First Light Image Launched January 6, 2003