ASTR 2310: Chapter 7, “The Sun” Observable Layers of the Sun  (Interiors deferred to Ch. 15, ASTR 2320)‏ Solar Activity Angular Momentum of the Sun.

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?
Chapter 8 The Sun – Our Star.
Chapter 16 Modeling the solar interior The vibrating sun Neutrinos Solar atmosphere: –Photosphere –Chromosphere –Corona Sunspots Solar magnetic fields.
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.
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 Sun Section 24.2 Pg The Sun  The sun is similar to most of the other stars in our galaxy  Large ball of gas made mostly of hydrogen and.
Chapter 7 The Sun. Solar Prominence – photo by SOHO spacecraft from the Astronomy Picture of the Day site link.
The star we see but seldom notice
The Sun- Our Star. The Sun- Our Star Star Parts: core radiation zone convection zone photosphere chromosphere corona solar wind.
The Sun The Sun in X-rays over several years The Sun is a star: a shining ball of gas powered by nuclear fusion. Luminosity of Sun = 4 x erg/s =
Conversations with the Earth Tom Burbine
+ The Sun. Sun Facts Makes life on our planet possible by giving us great amounts of light and heat Contains about 98% of the mass of the entire Solar.
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.
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,
THE SUN AND STARS And anything I want to put in here.
Astronomy 1020-H Stellar Astronomy Spring_2015 Day-30.
Our Sun. Why do we care about the Sun... - Light, heat, life - Space weather solar wind (1,000,000 mph) flares (UV, x-ray radiation) disturb Earth's magnetic.
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.
The Sun Internal structure of the Sun Nuclear fusion –Protons, neutrons, electrons, neutrinos –Fusion reactions –Lifetime of the Sun Transport of energy.
Chapter 20, Section 2 The Sun Anne Marie Scrudato’s notes borrowed by Rusty Sturken.
Chapter 9 The Sun. 9.4 The Active Sun Sunspots: appear dark because slightly cooler than surroundings:
The Sun: Our Star The Sun is an ordinary star and shines the same way other stars of its type do. The bright part normally seen is called the photosphere,
From the Core to the Corona – a Journey through the Sun
The Sun.
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.
SNC 1D1 – The Sun The sun and other celestial objects in the Universe emit electromagnetic radiation as part of the electromagnetic spectrum (EM spectrum).
By: Mrs. Greg Jennings.  Plasma is the fourth state of matter Liquid, solid, gas are the other three states Plasma is super-heated ionized gas.
OUR SUN THE CLOSEST STAR. Composition of the Sun The Sun is composed of at least 80 of the elements found on Earth. Sun is mostly composed of 91.2% Hydrogen,
The Sun’s Size, Heat and Temperature After completing this section, students will explain nuclear fusion, and describe the sun and compare it to other.
Visible Image of the Sun The Sun The Sun Our sole source of light and heat in the solar system A very common star: a glowing ball of gas held together.
The Sun 1 of 200 billion stars in the Milky Way. Our primary source of energy.
The Sun.
THE SUN. The Photosphere The Photosphere - The “visible” surface of the sun.  Thin layer of gas (less than 500km deep) from which we receive the majority.
Rotation Period = 25 days at the equator & 29 days near the pole Composition = 99% hydrogen and helium State = gaseous (plasma)
Ch. 26.1: Our Sun!.
The Sun Stellar Evolution: Low Mass Stars White Dwarfs
Solar Properties Has more than 99% the mass of our solar system Has more than 99% the mass of our solar system Diameter: 1,390,000 km Diameter: 1,390,000.
Chapter 9 Our Star, the Sun. What do you think? What is the surface of the Sun like? Does the Sun rotate? What makes the Sun shine?
1. Name one part of the sun. 2. Is the sun a solid, liquid or gas? 3. How hot was the center of the sun when it officially became a star?
The Sun, our favorite star!
THE SUN Energy from the sun, in the form of sunlight supports all life via photosynthesis, and drives the Earth’s climate and weather.
PHYS 1621 Proton-proton cycle 3 steps. PHYS 1622 Layers of the Sun Mostly Hydrogen with about 25% Helium. Small amounts of heavier elements Gas described.
Our Sun & Nuclear Fusion (Chapter 7). Student Learning Objectives Compare properties of the Earth and Sun Describe the layers of the Sun and how energy.
+ The Sun.
The Solar System. Nebula Theory (our solar system) The solar system started from the spinning and condensing of a cloud of dust and gas. The greatest.
The Sun: Part 2. Temperature at surface = 5800 K => yellow (Wien’s Law) Temperature at center = 15,000,000 K Average density = 1.4 g/cm 3 Density at center.
The Sun, our favorite star!
A105 Stars and Galaxies  Homework 6 due today  Next Week: Rooftop Session on Oct. 11 at 9 PM  Reading: 54.4, 55, 56.1, 57.3, 58, 59 Today’s APODAPOD.
Sun, Moon, Earth, How do they work together to help life survive? our sun.
ASTR 113 – 003 Spring 2006 Lecture 02 Feb. 01, 2006 Review (Ch4-5): the Foundation Galaxy (Ch 25-27) Cosmology (Ch28-39) Introduction To Modern Astronomy.
Outer Layers of the Sun Photosphere –Limb darkening –Sun spots Chromosphere Corona Prominences, flares, coronal mass ejections Reading
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 
The Sun.
(8th) Chapter 14-2 Cornell Notes
THE SUN.
Fusion vs Fission Fission Fusion Division of an atom’s nucleus
The Sun: Portrait of a G2V star
What is the fate of our sun and other stars?
How big is the Sun?. How big is the Sun? Our Sun is the LARGEST and BRIGHTEST body in the solar system The sun accounts for 99.8% of the solar system’s.
The Sun and Stars Lesson 2 pg. 808
The Sun.
24.3 The Sun Explain the structure of the Sun.
Do Now 12/9/09 What is the sun made of???
The Sun.
The Centre of the Solar System Earth Science 11
The sun gives off tremendous amounts of energy
Chapter 17 The Sun.
Sci. 2-2 The Sun: Our Very Own Star
Presentation transcript:

ASTR 2310: Chapter 7, “The Sun” Observable Layers of the Sun  (Interiors deferred to Ch. 15, ASTR 2320)‏ Solar Activity Angular Momentum of the Sun

ASTR 2310: Chapter 7, “The Sun” Observable Layers of the Sun Also see Wiki: Photosphere: where the light comes from (optical depth of 1), about the top 400 km, R=696,000km from the center. Absorption Lines indicate surface layer is cooler. Lines indicate H is 73.4% by mass, Helium 25.0%

ASTR 2310: Chapter 7, “The Sun” Atmospheric Opacity  Main source is the H - ion.  Hydrogen atom with an extra electron  Trace “metals” easily give up some outer electrons, partly ionized, and electrons are captured by neutral hydrogen to make ion  First electron ionization potential 13.6 eV, second only a mere 0.75 eV, so easily lost again, absorbs photons with wavlengths on order of 1.7 microns and shorter.  Need right range of densities and temperatures for this negative hydrogen ion to be common. Sun has them.

ASTR 2310: Chapter 7, “The Sun” Atmospheric Opacity  Limb Darkening: photons come from tau of 1, the photosphere. At the edge, that is from a shallower depth (and lower temperature) than in the center of the disk (T = 6100 K), for average of T = 5700 K.

ASTR 2310: Chapter 7, “The Sun” Other Atmospheric Phenomena  Granules that are convection cells (see movie on website on page 2 of the slides)‏  Chromosphere – hot, tenuous region above the photosphere with an emission-line spectrum, and temperature increasing with altitude  Other features include plages, filaments, prominences, and spicules

ASTR 2310: Chapter 7, “The Sun” Other Atmospheric Phenomena  Corona Very hot – into the millions of degrees Story of “Coronium” and forbidden Fe XIV Most easily seen in eclipses

ASTR 2310: Chapter 7, “The Sun” Other Atmospheric Phenomena  Corona and solar wind Origin of heating unclear, but acoustic and magnetic effects implicated Rms speed of corona particles (v rms = (3kT/m) 1/2 ) is on order a few hundred km/s Escape velocity (v esc =(2GM/r) 1/2 ) is a bit larger, but... The outer, hotter part of the corona has an increasing fraction of gas particles being lost  “Solar Wind” -- can make estimates on the whiteboard (from pages of the text)‏

ASTR 2310: Chapter 7, “The Sun” Solar Activity  Magnetic Fields and Lorentz Force Important for all solar activity Especially sunspots Some basic physics first (whiteboard)‏

ASTR 2310: Chapter 7, “The Sun” Solar Activity  Sunspots

ASTR 2310: Chapter 7, “The Sun” Solar Activity  Sunspots

ASTR 2310: Chapter 7, “The Sun” Solar Activity  Coronal Mass Ejections and Solar Flares, Auroras

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

© 2024 SlidePlayer.com. Inc. All rights reserved.