Solar Energy Transport & Luminosity

Similar documents
The Sun. How are these quantities measured? Properties of the Sun. Chapter 14

The Sun. Nearest Star Contains most of the mass of the solar system Source of heat and illumination

Sources of radiation

The Sun. The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x g = 330,000 M Earth = 1 M Sun

Problem Set 2 Solutions

What tool do astronomers use to understand the evolution of stars?

Announcements. - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11

Heat Transfer: A Practical Approach - Yunus A Cengel Assignment 11 Fall 2003 Tuesday, November 18, 2003 Chapter 11, Problem 49

The Interior Structure of the Sun

Astronomy 1 Fall Reminder: When/where does your observing session meet? [See from your TA.]

The Sun: A Star of Our Own ASTR 2110 Sarazin

Name... Class... Date...

Our Star: The Sun. Layers that make up the Sun. Understand the Solar cycle. Understand the process by which energy is generated by the Sun.

The Sun. Basic Properties. Radius: Mass: Luminosity: Effective Temperature:

The Sun Our Star. Properties Interior Atmosphere Photosphere Chromosphere Corona Magnetism Sunspots Solar Cycles Active Sun

1 Light from all distant galaxies is found to be shifted towards longer wavelengths. The more distant the galaxy, the greater the shift in wavelength.

Stars, Galaxies & the Universe Announcements. Stars, Galaxies & the Universe Observing Highlights. Stars, Galaxies & the Universe Lecture Outline

Teacher of the Week DEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS

The Sun. October 21, ) H-R diagram 2) Solar Structure 3) Nuclear Fusion 4) Solar Neutrinos 5) Solar Wind/Sunspots

MASSACHUSETTS INSTITUTE OF TECHNOLOGY Department of Physics Problem Solving 10: The Greenhouse Effect. Section Table and Group

Review from last class:

Chapter 9 The Sun. Nuclear fusion: Combining of light nuclei into heavier ones Example: In the Sun is conversion of H into He

aka Light Properties of Light are simultaneously

ASTRONOMY QUALIFYING EXAM August Possibly Useful Quantities

The Sun sends the Earth:

Tuesday, August 27, Stellar Astrophysics

Lecture 5: Greenhouse Effect

Radiation from planets

Lecture 5: Greenhouse Effect

Astronomy 1 Fall 2016

Lecture 3: Emission and absorption

Light and Matter(LC)

Some Good News. Announcements. Lecture 10 The Sun. How does the Sun shine? The Sun s Energy Source

PTYS/ASTR 206. The Sun 3/1/07

Chapter 5 Light and Matter: Reading Messages from the Cosmos. What is light? Properties of Waves. Waves. The Electromagnetic Spectrum

How the Sun Works. Presented by the

Greenhouse Effect & Habitable Zones Lab # 7

The greenhouse effect

Today in Astronomy 328

Atomic Physics 3 ASTR 2110 Sarazin

Outline. Astronomy: The Big Picture. Earth Sun comparison. Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned.

Astronomy 1 Winter 2011

Radiative Equilibrium Models. Solar radiation reflected by the earth back to space. Solar radiation absorbed by the earth

Opacity. requirement (aim): radiative equilibrium: near surface: Opacity

Proton-proton cycle 3 steps PHYS 162 1

1. Solar Atmosphere Surface Features and Magnetic Fields

10/27/2017 [pgs ]

Name: Date: 2. The temperature of the Sun's photosphere is A) close to 1 million K. B) about 10,000 K. C) 5800 K. D) 4300 K.

8.5 GREENHOUSE EFFECT 8.6 GLOBAL WARMING HW/Study Packet

B B E D B E D A C A D D C

ME 476 Solar Energy UNIT TWO THERMAL RADIATION

Today. Spectra. Thermal Radiation. Wien s Law. Stefan-Boltzmann Law. Kirchoff s Laws. Emission and Absorption. Spectra & Composition

Spectrum of Radiation. Importance of Radiation Transfer. Radiation Intensity and Wavelength. Lecture 3: Atmospheric Radiative Transfer and Climate

Astro Week 1. (a) Show that the transit duration for a non-central transit (see Figures) is: R R. b = a cos i

Book page cgrahamphysics.com Stellar Spectra

ASTR-1010: Astronomy I Course Notes Section IV

Earth s orbit. 2.2 Celestial mechanics. Earth s orbit. Earth s orbit. Variation of eccentricity over Earth s history. 0 e 1

Today in Astronomy 111: the Sun and other blackbodies

Today The Sun. Events

Light and Atoms. ASTR 1120 General Astronomy: Stars & Galaxies. ASTR 1120 General Astronomy: Stars & Galaxies !ATH REVIEW: #AST CLASS: "OMEWORK #1

Lecture 3: Atmospheric Radiative Transfer and Climate

Supporting Calculations for NASA s IRIS Mission. I. Overview

Astronomy 1102 Exam #1 Chapters 1,2,5,6 & 16

Next quiz: Monday, October 24

AST 301, Lecture 2. James Lattimer. Department of Physics & Astronomy 449 ESS Bldg. Stony Brook University. January 29, 2019

Chapter 16 Lecture. The Cosmic Perspective Seventh Edition. Star Birth Pearson Education, Inc.

Energy. Kinetic and Potential Energy. Kinetic Energy. Kinetic energy the energy of motion

Atoms and Star Formation

Stellar Astronomy Sample Questions for Exam 3

Astronomy 1504 Section 002 Astronomy 1514 Section 10 Midterm 2, Version 1 October 19, 2012

Ay Fall 2004 Lecture 6 (given by Tony Travouillon)

Star-Forming Clouds. Stars form in dark clouds of dusty gas in interstellar space. The gas between the stars is called the interstellar medium.

Lasers PH 645/ OSE 645/ EE 613 Summer 2010 Section 1: T/Th 2:45-4:45 PM Engineering Building 240

Today. Kirchoff s Laws. Emission and Absorption. Stellar Spectra & Composition. Doppler Effect & Motion. Extrasolar Planets

Lec 7: Classification of Stars, the Sun. What prevents stars from collapsing under the weight of their own gravity? Text

Lecture 5: As Long as the Sun Shines. Temperature of the Sun. Spectrum of the Sun Sunspots. Chromosphere. Sodium. Hydrogen.

SISD Training Lectures in Spectroscopy

Earth: the Goldilocks Planet

In class quiz - nature of light. Moonbow with Sailboats (Matt BenDaniel)

The Sun Closest star to Earth - only star that we can see details on surface - easily studied Assumption: The Sun is a typical star

Chapter 5 Light and Matter: Reading Messages from the Cosmos

Lecture 4: Radiation Transfer

Today. Homework Due. Stars. Properties (Recap) Nuclear Reactions. proton-proton chain. CNO cycle. Stellar Lifetimes

Oppgavesett kap. 4 (1 av 2) GEF2200

Electromagnetic Radiation. Physical Principles of Remote Sensing

Electromagnetic Radiation. Radiation and the Planetary Energy Balance. Electromagnetic Spectrum of the Sun

The current climate epoch: The Holocene

Hydrogen Burning in More Massive Stars.

! The Sun as a star! Structure of the Sun! The Solar Cycle! Solar Activity! Solar Wind! Observing the Sun. The Sun & Solar Activity

Chapter 5 Light and Matter: Reading Messages from the Cosmos. How do we experience light? Colors of Light. How do light and matter interact?

Astronomy Ch 16 The Sun. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Astronomy 210. Outline. Nuclear Reactions in the Sun. Neutrinos. Solar Observing due April 15 th HW 8 due on Friday.

Solar radiation - the major source of energy for almost all environmental flows

Lecture 4: Global Energy Balance. Global Energy Balance. Solar Flux and Flux Density. Blackbody Radiation Layer Model.

Lecture 4: Global Energy Balance

Introduction to the Sun

Stars AS4023: Stellar Atmospheres (13) Stellar Structure & Interiors (11)

Electromagnetic Radiation.

1 A= one Angstrom = 1 10 cm

Stars, Galaxies & the Universe Lecture Outline

Transcription:

Solar Energy ranort & Luminosity Energy transer rom core to solar surace by radiative tranort mode ollowed by convective energy tranort! Luminosity in erg/s: L r r 2 r (r) is energy lux in erg s - cm -2 at radius r M core 0.M With: L =3.87 0 33 erg/s = 6.32 0 0 erg s - cm -2 or R =6.96 0 0 cm

Black Body Radiation o the Sun Black bodies have 00% absorption o photons and zero relectivity! he sun, stars and all stellar objects are treated as black bodies! Energy lux or black bodies is described by Stean Boltzmann law: = 5.67 0-5 erg s - cm -2 K - = 5.67 0-8 W m -2 K - (Stean s constant) Planck unction describes the ectral distribution o a black body o temperature B ( ) 3 2h 2 c h k e Planck constant: h=6.625 0-3 J s Boltzmann constant: k=.38 0-23 J K - c k c k hc E h : requency : wavelength k: wavenumber hc k 8 W MW 0 erg 5.670 6000K 73.5 7.350 sun 2 2 m K m cm 2 s

emperature dependence o solar lux he solar lux or the luminosity depends very sensitively on the temperature ( )! Emission rom cooler areas is reduced! Wien s law: the peak o the lux distribution depends on the temperature! 2897 m max

Homework 2 Calculate the Planck unction B () and the wavelength max or maximum radiation emission or earth assuming an average surace temperature o 280K.

Solar constant 0 = (R /R orbit ) 2 R = 6.96 0 5 km = 0.0065 AU R orbit =.96 0 8 km = AU 0 = (R /R orbit ) 2 = 6.32 0 0 erg s - cm -2 (R /R orbit ) 2 = 2.6 0-5 0 =.37 0 6 erg s - cm -2 lux=solar Constant: 0 =.366 0 3 W/m 2, R earth = 637 km Solar power incident on earth: S 0 = R earth2 0 =.7 0 7 W

Variations o solar constant lux Irridiance Measurements o solar constant over last 30 years indicate variation o 0.03% Model based reconstruction o long term irradiance suggests slight increase by 0.0%. A regular oscillation o 0.0% is observed in an eleven year cycle!

Sun ots Sun ots are correlated to strong magnetic ields breaking through the photohere o our sun! Granule 5800 K Penumbra 5500 K Umbra 500 K Outlow o material along magnetic ield lines rom inner to outer penumbra sunots are associated with increased cosmic ray intensity (highly ionized particles) Magnetic ield at center is vertical, at outer penumbra it becomes horizontal Magnetic ield strength B drops rom 2000-000G towards boundary strong magnetic ields quench convective motion reduce energy tranort opacity changes with temperature, through sunots one can see deeper

Sunot cycles years Maunder minimum

Solar cycle and cosmic ray lux # o sunots n N(n,p) C rel. C concentration years Decline o C equilibrium content in Atmohere. Why? year C concentration in Georgian wine during the 0 year period o 908 to 952 shows direct correlation with sunot activity, similar observations with old whisky!

Quick and dirty example he average sunot has a diameter o 500 km (large ones can reach the size o earth diameter) and a temperature o = 500 K. he anular solar surace has an average temperature o = 5800 K. he solar energy lux and solar power reaching earth at a time o low sunot activity is 365.5 W/m 2 compared to a lux o 366.5 W/m 2 at a time o maximum sunot activity? Estimate the raction o the sun covered by sunots! 3 0.5 5800 500 366.5 365.5 quiet active quiet active quiet active quiet active 0.%

3 5 2 2 2 0 5 0 5 00 70000 500 00 70000 500 km km km km n R r n A A n sun sun A /2 =7.7 0 km 2

he uture o the Sun or the ultimate climate change in ~ 6-8 Billion years According to solar model simulations the hydrogen content in our sun has declined to about 50% o the initial value, we run low in uel! Hydrogen burning zone expands outward, orcing the sun to expand! he solar here ows slowly enguling the inner planets, causing the ultimate global warming on earth!

he movie to the book he inal global warming scene!

he ectra o the stars depend on composition, density, and temperature o the stellar atmohere. Atoms in the atmohere absorb light emitted at lower layers and produce the dark vertical lines or bands in the ectrum. Solar ectrum