* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Download Lecture 10: Stars
Leibniz Institute for Astrophysics Potsdam wikipedia , lookup
Geocentric model wikipedia , lookup
Aries (constellation) wikipedia , lookup
Chinese astronomy wikipedia , lookup
Auriga (constellation) wikipedia , lookup
Extraterrestrial life wikipedia , lookup
Canis Minor wikipedia , lookup
Corona Borealis wikipedia , lookup
Rare Earth hypothesis wikipedia , lookup
History of astronomy wikipedia , lookup
Cassiopeia (constellation) wikipedia , lookup
Cygnus (constellation) wikipedia , lookup
Constellation wikipedia , lookup
Theoretical astronomy wikipedia , lookup
Corona Australis wikipedia , lookup
Dialogue Concerning the Two Chief World Systems wikipedia , lookup
International Ultraviolet Explorer wikipedia , lookup
Canis Major wikipedia , lookup
Perseus (constellation) wikipedia , lookup
Astronomical unit wikipedia , lookup
Aquarius (constellation) wikipedia , lookup
Star catalogue wikipedia , lookup
Future of an expanding universe wikipedia , lookup
Malmquist bias wikipedia , lookup
H II region wikipedia , lookup
Stellar evolution wikipedia , lookup
Corvus (constellation) wikipedia , lookup
Timeline of astronomy wikipedia , lookup
Observational astronomy wikipedia , lookup
Cosmic distance ladder wikipedia , lookup
Star formation wikipedia , lookup
2/13/14 ASTR 1040: Stars & Galaxies Eskimo Planetary Nebula Topics for Today & Tues & What can we measure in other stars? & How do we begin to classify other stars? & Vital work by Annie Jump Cannon in devising a sensible “spectral sequence” for stars & Why temperature and spectral lines are closely linked in classifying stars O B A…M Prof. Juri Toomre TA: Ryan Orvedahl Lecture 10 Thur 13 Feb 2014 zeus.colorado.edu/astr1040-toomre Logistics Chap 15 – SURVEYING THE STARS & Read Chap 15.1: Properties of Stars & Overview read for recitation Chap S3: Spacetime & Gravity (Black Holes) & First Mid-Term Exam in class today (9:50am) -- 50 minutes & Observatory #3 was last night & Homework #4 due on in class on Tues & Fiske Planetarium next Thur (20 Feb) on “Black Holes: Other Side of Inifinity” Often only seeing a point of light & Stars are so small compared to their distance that we almost never have the resolution to see their sizes and details directly – “point sources” & We deduce everything by measuring the amount of light (brightness) at different wavelengths (color, spectra) & Measuring stellar luminosities & Measuring distances & Measuring temperatures So what can we find out about other stars? APPARENT BRIGHTNESS POSITION SPECTRUM 1 2/13/14 Most Basic Problem in Astronomy Inverse Square Law of Brightness Apparent Brightness ≈ Lo / (distance)2 Star of given APPARENT BRIGHTNESS could be either A. very luminous star far away B. low luminosity star closer by Need to know the DISTANCE to the star Stellar Luminosity & What we measure: APPARENT BRIGHTNESS or how bright it appears to us here on Earth & What we want to know: (absolute) LUMINOSITY or how much energy is emitted (joules/sec or watts) Parallax – to determine distance o Measure the apparent movement of stars over a year o Movement is caused by Earth’s movement around the Sun o Closer objects will move more than farther objects & Need to know DISTANCE to the star How Stellar Parallax Works Class self-demo of parallax & Your nose is the Sun & Your left eye is the Earth in January & Your right eye is the Earth in June Watch the apparent motion of your thumb against a distant reference point (repeat at arm’s length) Which “move” more -- closer or farther objects? 2 2/13/14 Stellar Parallax: measuring nearby distances Best parallax measurers: Hipparcos satellite 1989-1993 GAIA satellite Dec 2013 à & Space measurements not affected by atmosphere & Measurement made many times until accurate to ~0.001 arcsec (Hipparcos à1,600 light years) & 100,000 stars mapped; 2.5 million lesser accuracy & GAIA: 10 micro-arcsec, billion stars; 10,000+ ly Spectra help classify stars Measuring Surface TEMPERATURE Shape of spectrum good … but spectral lines much better OBAFGKM ?!? & Spectral (color) classification O = bluest, hottest G = yellow (Sun) M = reddest, coolest A bit of history: Classifying Stars World War I, Harvard College observatory Women were hired by Pickering as “calculators” to help with a new survey of the Milky Way Most had studied astronomy, but were not allowed to work as scientists 3 2/13/14 Devising the strange temperature code Which absorption (dark) lines are strongest? & Original classification of spectra (1890) was: A = strongest hydrogen feature B = less strong hydrogen …C, D, etc. & Annie Jump Cannon realized that a different sequence made more sense (~1910) à O B A F G K M !! Spectral Classification: O B A F G K M Which ABSORPTION lines are strongest First Mid-Term Exam Hottest stars: O B ionized helium only Hot stars: A F helium, hydrogen Cooler stars: G hydrogen, heavier atoms Coolest stars: M molecules, (complex absorption bands) Rules of the Game & Closed book, closed notes, can use doublesided handwritten “crib sheet”; 50 minutes & Print your name and student ID on top of pages 1 and 6 of exam sheets & Print and encode your name and student ID on scan sheet (and nothing else) & Use # 2 (soft) pencil for marking your answers on scan sheet ($ 1 buys you a pencil !) & Respond carefully to Essay Question 46, with full and lucid sentences (even a sketch or two) 4