Solar-Stellar Connection

Slides:

Advertisements

Similar presentations

EQ: WHAT IS SUNLIGHT?. Photon Absorption and Emission Photon Continuous stream of photons (light) emitted by energized vibrating electrons. Wavelengths.

Advertisements

Energy Production in the Sun Physics 113 Goderya Chapter(s): 8 Learning Outcomes:

Electromagnetic Radiation Electromagnetic radiation - all E-M waves travel at c = 3 x 10 8 m/s. (Slower in water, glass, etc) Speed of light is independent.

The Sun, our favorite star! WE CAN SEE IT REALLY WELL. The Sun is the basis for all of our knowledge of stars. Why?

Solar Radiation Emission and Absorption

Chapter 6 Atoms and Starlight.

The star we see but seldom notice

AST 444 Problems.

Announcements Star Assignment 4, due Monday March 22 ÜDo Angel quiz, Quiz 2: Monday March 22 Light, Planets, Sun, Observations of stars Chapters 6.4-5,

The Sun. Overview 1.What is the composition of the Sun? 2.Why does the Sun shine? 3.How do we know its temperature? 4.Why is the Sun hot? (what’s it’s.

Properties of Stars How do we measure stellar luminosities?

Properties of Stars. Distance Luminosity (intrinsic brightness) Temperature (at the surface) Radius Mass.

Stars Introduction To “Atomic Astrophysics and Spectroscopy” (AAS) Anil Pradhan and Sultana Nahar Cambridge University Press 2011 Details at:

AST 111.  The Sun is the STAR at the center of the Solar System  Anything else belonging to the Solar System is NOT a star!

Today’s APODAPOD  Read Chapter 11  Homework and Quiz 9 this week on Friday  Last Solar Lab on TOMORROW at NOON The Sun Today A100 The Sun.

The Sun Goals: -Summarize the overall properties of the Sun.

Now we begin…..

Analyzing Starlight 1)Blackbody radiation 2)Properties of Stars 3)Measuring the Properties of Stars 4)H-R diagram October 16, 2002.

Red Stars, Blue Stars, Old Stars, New Stars Session 1 Julie Lutz University of Washington.

Radiation Kirchoff’s Laws  Light emitted by a blackbody, a hot opaque body, or hot dense gas produces a continuous spectrum  A hot transparent gas produces.

The Sun – A typical Star The only star in the solar system Diameter: 110  that of Earth Mass: 300,000  that of Earth Density: 0.3  that of Earth (comparable.

Measuring the Stars How big are stars? How far away are they?

PHYS 205 Powerhouse PHYS 205 Possible sources Chemical Energy: Sun has hydrogen and if it has oxygen, than we can make water. will last 18,000 years.

 The sun has a very high temperature of degrees Fahrenheit. It is made of 70% Hydrogen, 28% helium, and 2% metals. It has no moons although it.

1 II-6 Stellar Mass and Binary Stars (Main Ref.: Lecture notes; FK Sec.4 - 4, 6, 7; 17-9, 10, and 11, Box 4-2, 4-4) II-6a. Introduction If the star is.

Definition: All space and objects within the Sun’s gravitational influence. (sun is sol, helios)

Properties of Stars.

PHYS More about Electromagnetic Radiation Speed of light = frequency  wavelength = a constant c Q. How do we generate light? A. Heat things up.

Stars Other Suns. Physical Properties Luminosity Mass Diameter (radius) Must know distance to find out these properties!

The Sun and the Solar System Chapter Sun’s Size, Heat and Structure Diameter= 1,400,000 km or 868,000 miles –More than 3x the distance of Earth.

{ Week 22 Physics.  Understand that a star is in equilibrium under the action of two opposing forces, gravitation and the radiation pressure of the star.

Ch. 12 Lesson 1 Stars. What are stars? A star is large ball of gas that emits (gives off) energy produced by nuclear reactions in the star’s interior.

Stars come in all sizes, small, large and even larger.

The Solar System Missions. planets not shown to scale >> MercuryVenusEarthMarsJupiterSaturnUranusNeptunePluto Mean Distance from the Sun (AU)

Measuring the Stars What properties of stars might you want to determine?

The Sun and the Inner Planets. THE SUN -The Sun is the Largest object in our solar system. -The Greeks called it Helios, the Romans called it Sol. The.

Blackbody Radiation A blackbody is something that absorbs all radiation that shines on it Are all blackbodies black? - no!! - imagine a box full of lava.

Properties of Stars. "There are countless suns and countless earths all rotating around their suns in exactly the same way as the seven planets of our.

Measuring Stars. Visible Spectrum & Wavelengths Spectral Types Continuous spectrum: Produced when white light passes through a prism Emission spectra:

Proton-proton cycle 3 steps

12-1 Notes - Stars Chapter 12, Lesson 1.

Class Notes for Monday, Feb 20th

Integrated Science Unit 11, Chapter 31.

Measuring the Astronomical Unit

Stars Luminous gaseous celestial body – spherical in shape held by its own gravity.

Inner Solar System (Terrestrial Planets)

Unit 1 Physics Detailed Study 3.2

Integrated Science.

The Sun – A typical Star The only star in the solar system

The Sun The Sun’s Spectrum

Temperature, Color, Radius

The Sun: Our Star.

The Characteristics of Stars

The Properties of Stars

Arinto Yudi Ponco Wardoyo

Modeling Stars.

Measuring the Astronomical Unit

Ch. 26 The Sun and the Solar System

The Solar-Stellar Connection

Radiation Kirchoff’s Laws

Chapter 17 The Sun.

Newton’s Law of Universal Gravitation

The Sun and Stars.

The colour of A star changes depending on it’s temperature

The Properties of Stars

Presentation transcript:

Solar-Stellar Connection The Sun: Home Star Solar-Stellar Connection

The Sun Key to solar-stellar connection Close-up model for other stars Local “lab” for testing ideas about the physics of stars Energy source for most life on earth

Must know distance to find these! Sun: Properties Luminosity Mass Radius Must know distance to find these!

Analyze spectrum to find these; do not need to know distance! Sun: Properties Surface temperature Chemical composition Analyze spectrum to find these; do not need to know distance!

Distance 1 AU! About 150 million km How? Bounce radar signals off Venus! Know distance in AU from Kepler’s laws. Know speed of light, measure travel time => distance in km, known fraction of AU; get AU in km

Luminosity At earth, measure flux: Energy passing through an area per second => 1370 W/s Imagine a sphere around the sun with radius 1 AU Collects 4 x 1026 W, sun’s luminosity or power

Mass Apply: Newton’s version of Kepler’s 3rd or Newton’s 2nd law plus law pf gravitation Need earth’s orbital period (365 days) and distance, 150 million km (1 AU) Result: 2 x 1030 kg, 330,000 times that of earth

Diameter (Radius) Angular diameter from earth about 1/2 degree => actual diameter/distance = 1/110 Know distance (1 AU in km) Actual diameter = (1/110) x 150 x 106 km = about 1.4 million km, or 100 times earth!

Chemical Composition Absorption-line spectrum: Match lines to those of known elements Information only about photosphere, where lines form Mostly H (72%) and He (26%)

Surface Temperature Assume: Radiates like a blackbody (Planck curve of continuous emission) Then: Match overall curve or use peak of emission Get: Temp about 5800 K

Solar Energy Source: Fusion reactions (H => He) in core, where temperature 10 to 15 million K How: E = mc2; thermonuclear reactions convert mass to energy (heat & light) Energy flow: From core to surface takes light about 200,000 y (opaque!)