X Visit www.worldofteaching.comwww.worldofteaching.com For 100’s of free powerpoints.

Slides:



Advertisements
Similar presentations
The Science of Solar B Transient phenomena – this aim covers the wide ranges of explosive phenomena observed on the Sun – from small scale flaring in the.
Advertisements

Solar Theory (MT 4510) Clare E Parnell School of Mathematics and Statistics.
Sun Mr. Skirbst Physical Science Topic 26. The Sun.
Chapter 22 Test Review.
Chapter 8 The Sun – Our Star.
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.
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.
Instructor Notes These images correspond to the layers of the Sun discussed in the Features of the Sun – 3D Sun lesson. Layers – Photosphere:
Instructor Notes There is one picture of the Sun in all wavelengths except: Gamma ray – there are no images of the full Sun in gamma ray.
Magnetic fields in the photosphere and heliosphere: structure, statistical parameters, turbulent state Valentyna I. Abramenko Big Bear Solar Observatory.
High-latitude activity and its relationship to the mid-latitude solar activity. Elena E. Benevolenskaya & J. Todd Hoeksema Stanford University Abstract.
Chapter 7 The Sun. Solar Prominence – photo by SOHO spacecraft from the Astronomy Picture of the Day site link.
Solar-B XRT XRT-1 The Science and Capability of the Solar-B / X-Ray Telescope Solar-B XRT Presenter: Ed DeLuca Smithsonian Astrophysical Observatory.
Connecting coronal structure to photospheric origins Active region (sunspot) evolution and solar rotation well define long term, persistent, coronal streamers.
Coronal holes as seen in soft X-rays H. S. Hudson (UCB and SPRC) SOHO-11, Davos, March 13, 2002.
Physics 681: Solar Physics and Instrumentation – Lecture 25 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research.
Review of Conditions for the Formation and Maintenance of Filaments Paper by Sara F. Martin, 1998 Review presented by Samuel Tun October 13, 2005
The active Sun. The magnetic Sun White lightMagnetic field.
How The Sun Works Brady Gurley. The Sun: What it’s made of -~70% Hydrogen -~28% Helium -~1.5% Carbon, Nitrogen, & Oxygen -~0.5% Other Elements (Neon,
Conversations with the Earth Tom Burbine
The Layers of a Star The corona is the wide, outermost layer of a Sun’s atmosphere – (AL) The chromosphere is the orange-red layer of the Sun’s atmosphere,
Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.
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.
Note key, please leave in binder. Our Sun
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,
Transition Region And Coronal Explorer Observes three-dimensional magnetic structures in the Photosphere Defines the geometry and dynamics of the Transition.
Three Dimensional Visualization of the Solar Corona and study of coronal cavity observed by Yohkoh/SXT and Hinode/XRT J. Okumura, D. Mineyama, H. Watanabe,
The Sun. Solar Prominence Sun Fact Sheet The Sun is a normal G2 star, one of more than 100 billion stars in our galaxy. Diameter: 1,390,000 km (Earth.
Chapter 9 The Sun. 9.4 The Active Sun Sunspots: appear dark because slightly cooler than surroundings:
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.
SLIDE SHOW 3 B changes due to transport + diffusion III -- * * magnetic Reynold number INDUCTION EQUATION B moves with plasma / diffuses through it.
SHINE SEP Campaign Events: Long-term development of solar corona in build-up to the SEP events of 21 April 2002 and 24 August 2002 A. J. Coyner, D. Alexander,
The Sun- Solar Activity. Damage to communications & power systems.
The Solar Wind.
SUN, EARTH AND SPACE. THE SUN CLOSE UP: INSIDE AND OUT.
SOLAR FLARES AND ERUPTIONS Lyndsay Fletcher University of Glasgow.
The Sun The Sun imaged in white light by the SOHO spacecraft.
© 2010 Pearson Education, Inc. Solar Thermostat Decline in core temperature causes fusion rate to drop, so core contracts and heats up. Rise in core temperature.
Our Sun 93 million miles from Earth 150 million kilometers Earth 99.8% of the mass of our solar system.
The Sun – Our Star Our sun is considered an “average” star and is one of the 100 BILLION stars that make up the Milky Way galaxy. But by no MEANS does.
Dr Dash will be on travel for the next two weeks (off to Africa). We will have a guest lecturer and Justin will be available to answer questions. Homework.
The Sun Diameter is 110 times Earth’s Mass is 745 times Earth’s
The Sun appears to have been active for 4.6 billion years and has enough fuel to go on for another five billion years or so.
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,
Sun Lesson 3. Sun The sun is a star located at the center of our solar system. The nearest star from earth and our engine for life. It is a medium-sized.
Sun, Moon, Earth, How do they work together to help life survive? our sun.
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.
The Sun…a star in our solar system (continued). But first…see a solar twin tonight Beta Canum Venaticorum…look almost up and a little east at 9PM.
The Sun. The Sun.  Is located in the outer bands of our Galaxy  Is the center of our Solar System  Is a STAR!!!  Rotation: once in about 25 days 
Our Sun. About the Sun The sun is by far the largest object in the solar system, containing more than 99.8% of the total mass of the solar system (Jupiter.
The Sun. Sun Fact Sheet The Sun is a normal G2 star, one of more than 100 billion stars in our galaxy. Diameter: 1,390,000 km (Earth 12,742 km or nearly.
© 2017 Pearson Education, Inc.
Topic: The Sun PSSA: D/S8.D.3.1.
Solar atmosphere.
Sun Notes.
CORONAL LOOPS.
The sun’s gravity holds all of the planets and comets in orbit
The Sun: Portrait of a G2V star
The Sun: close-up of a spectral class G main sequence star
The Sun and Stars Lesson 2 pg. 808
The Sun Our Nearest Star
The Sun Chapter 17.
Section 2: Solar Activity
The Sun & It’s Solar System
Solar and Heliospheric Physics
The Sun.
Ron Moore and Alphonse Sterling
The Sun and Other Stars 14-2.
Sun Lesson 3.
The Sun.
Presentation transcript:

X Visit For 100’s of free powerpoints

X-Rays Above left, our galaxy in X-rays, above, a supernova

The Observatory

Yohkoh SXT & Team Specs 1.54m focal length provides images from the.25 to 4.5 keV on a 1024x1024 cdc detector

Yohkoh Assembly

Yohkoh X-Ray Pictures

The Corona

Active Region Caused by strong magnetic fields that may span up to 500,000 square kilometers

Arcade of loops “An "arcade" is a system of magnetic loops organized into an elongated cylindrical formation. Often such an arcade will result from a slowly-developing solar flare or a coronal mass ejection (or both). The bright arcade may persist for days or longer.”

X-Ray Bright Points These occur anywhere on the Sun at opposition of the active regions. Caused by magnetic fields that are sucked down into the photosphere

Corona Hole unipolar magnetic fields high-speed solar wind streams originate in coronal holes

Interconnecting loops large-scale magnetic loops connect two active regions "emerging flux": magnetic loops push their way through the photosphere and appear in the corona

Streamer The result of two opposed arcades resulting in explosions of x-rays from the sun

The MAXIM

Interferometry Above: Hawaii’s twin Keck observatories Below: New Mexico’s Very Large Array

The MAXIM

MAXIM

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2025 SlidePlayer.com. Inc. All rights reserved.