Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.

Slides:



Advertisements
Similar presentations
PHOTOSPHERE The lowest layer of the Suns atmosphere that is also the visible part we see.
Advertisements

What is the fate of our sun and other stars?
Institute for Gravitational Research
The Sun The Sun is a star. The Sun is a star. It is 4,500 million years old It is 4,500 million years old It takes 8 minutes for its light to reach.
This work was performed under the auspices of the Significant Opportunities in Atmospheric Research and Science Program. SOARS is managed by the University.
The Sun’s Dynamic Atmosphere Lecture 15. Guiding Questions 1.What is the temperature and density structure of the Sun’s atmosphere? Does the atmosphere.
This work was performed under the auspices of the Significant Opportunities in Atmospheric Research and Science Program. SOARS is managed by the University.
Review Vocabulary magnetic field: the portion of space near a magnetic or current-carrying body where magnetic forces can be detected The Sun contains.
The Hunt for a Link : Quantitative Connections Between Magnetic Fields and EIT Coronal Wave/CME Properties Prepared by James R. Robertson J.R. In conjunction.
Alfvén Waves in the Solar Corona S. Tomczyk, S. Mclntosh, S. Keil, P. Judge, T. Schad, D. Seeley, J. Edmondson Science, Vol. 317, Sep., 2007.
Magnetic Activity Astronomy 315 Professor Lee Carkner Lecture 11.
The Sun- Our Star. The Sun- Our Star Star Parts: core radiation zone convection zone photosphere chromosphere corona solar wind.
The active Sun. The magnetic Sun White lightMagnetic field.
Conversations with the Earth Tom Burbine
Is There Life Out There? Our Solar System (and beyond) Draw a picture of what you think life would look like on another planet, if it existed. Describe.
Coronal Mass Ejection Also known as CME CMEs are huge bubbles of gas within magnetic field lines that are ejected from the Sun over the course of several.
The Sun a medium sized star 93,000,000 miles away 109 times diameter of Earth 1 million Earths could fit in the Sun Made of gas: 82% hydrogen, 17% helium,
Our Sun A medium sized star. Our Sun Our sun is a typical medium sized star. A star is a hot ball of plasma that shines because nuclear fusion is taking.
The Sun Earth Science - Mr. Gallagher. The Sun is the Earth's nearest star. Similar to most typical stars, it is a large ball of hot electrically charged.
Structure & Function. Our Nearest Star  Core  Comprises about 25% of sun’s interior  site of nuclear fusion  Radiative Zone  Energy produced in.
The Sun as a Star The “Surface” of the Sun and Its Structure Outer Layers – 3 distinct region Photosphere Chromosphere Corona.
The Sun The Sun is a star Huge ball of glowing ionized gas… plasma. Gravity vs. Nuclear Fusion Gravity wants to crush the star Fusion wants to explode.
Chapter 26 Relativity. General Physics Relativity II Sections 5–7.
Curtis Walker – UCAR/SOARS/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.
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:
The Sun By: Kristel Curameng and Courtney Lee. The Sun The Sun is the most prominent feature in our solar system. The largest object and contains approximately.
Survey of the Universe Tom Burbine
The Solar Interior Core Radiation Zone Convection Zone.
The Sun ROBOTS Summer Solar Structure Core - the center of the Sun where nuclear fusion releases a large amount of heat energy and converts hydrogen.
The Sun Astronomy 311 Professor Lee Carkner Lecture 23.
The SUN!.
By Elisha. » The Sun » The sun is the star in the centre of the solar system in which the earth orbits around and is about 149,600,000 km away from earth.
This work was performed under the auspices of the Significant Opportunities in Atmospheric Research and Science Program. SOARS is managed by the University.
SOLAR FLARES AND ERUPTIONS Lyndsay Fletcher University of Glasgow.
The Sun Stellar Evolution: Low Mass Stars White Dwarfs
OUR SUN. Solar Nebula: - Cloud of gas and dust that developed into the solar system. - Our Sun was developed as a star from the burning of Hydrogen gas.
Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.
The Sun Diameter is 110 times Earth’s Mass is 745 times Earth’s
The Sun, our favorite star!
Our Sun.
Unit 8 Chapter 29 The Sun. We used to think that our sun was a ball of fire in the sky. Looking at our sun unaided will cause blindness. The Sun’s Energy.
Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.
Sun Notes. Characteristics CLOSEST star to earth CLOSEST star to earth The bright star in the center is Proxima Centauri.
Our Star the Sun. The Sun – Our Star Our sun is considered an “average” star and is one of the 200 BILLION stars that make up the Milky Way galaxy. But.
Curtis Walker – UCAR/SOARS Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.
NOTES: The Sun How big? D(Jupiter) = 10 x D(Earth) D(Sun) = 10 x D(Jupiter) More precisely, D(Sun) = 109 x D(Earth). (See overlay) Or 1.3 million Earth.
Outer Layers of the Sun Photosphere –Limb darkening –Sun spots Chromosphere Corona Prominences, flares, coronal mass ejections Reading
THE SUN The star we see by day.
The Sun as a Star The “Surface” of the Sun and Its Structure
Section 1: The Sun The Sun contains most of the mass of the solar system and has many features typical of other stars. K What I Know W What I Want to.
By Katie Licheni and Paige Lemura, 7G
THE SUN.
Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO
PROPERTIES OF THE SUN Essential Questions
Section 1: The Sun The Sun contains most of the mass of the solar system and has many features typical of other stars. K What I Know W What I Want to.
THE SUN AS AN ENERGY SOURCE
Solar Activity and Space Weather
What is the fate of our sun and other stars?
Properties of the Sun Visual Vocabulary.
Photometric Analysis of Asteroids
Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO
The Sun.
Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO
The Sun.
OUR SUN.
Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO
Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO
By: Dani Steele and Shayna Richards
Information to annotate Diagram.
Presentation transcript:

Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO

 Sun’s “Atmosphere”  1 million degree Kelvin plasma  Can only be seen during total solar eclipse  May be viewed with coronagraphs outside of eclipse  Emits massive quantities of energy  Origin of the Solar Wind Image Courtesy of Google Images

 Instrumentation that produces a false eclipse of the sun allowing coronal observation  Ground-based and satellite-based varieties Images Courtesy of Google Images

 Dark Frame Corrections  Flat Field Corrections  Aerosol Removal

 Thresholding the images by three different techniques  Median Array  Mean Array  Minimum Array

 We have successfully removed aerosols from an image utilizing one technique  We will still attempt other techniques for comparison

 Scott Sewell NCAR/HAO  Steve Tomczyk NCAR/HAO  Amy Stevermer UCAR/COMET  Theresa Aguilar UCAR/Texas Tech

For the time being these are my concerns and observations: 1.How much educational (corona and coronagraph) information is necessary since our audience is not solar physict? 2.There should be some slide towards the beginning that explains what I am doing and why…? 3.I question the necessity of CCD vs. CMOS discussion…? 4.I certainly already feel the time crunch…?

CCDCMOS/SCMOS  Charge coupled-device  Converts photons into electrons which become the image signal  (Scientific) Complementary metal-oxide-semiconductor  Greater efficiency