Chapter 29 Notes
... • Parallax is used to find the distance to stars • Constellations: Groups of stars in the same part of the sky • Clusters: groups of stars bound together by gravity • Binaries: two stars that orbit a common center of mass ...
... • Parallax is used to find the distance to stars • Constellations: Groups of stars in the same part of the sky • Clusters: groups of stars bound together by gravity • Binaries: two stars that orbit a common center of mass ...
Name____________________________________________
... S6E1 Where do we live in the Universe, Milky Way, and our Solar System? 1. Between 15-20 billion years ago the Universe began expanding out of an enormous explosion scientist called the Big Bang theory. 2. From largest to smallest, order the following (1 is largest -4 is smallest): __4___ The Sun __ ...
... S6E1 Where do we live in the Universe, Milky Way, and our Solar System? 1. Between 15-20 billion years ago the Universe began expanding out of an enormous explosion scientist called the Big Bang theory. 2. From largest to smallest, order the following (1 is largest -4 is smallest): __4___ The Sun __ ...
Life Cycle of Stars
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a large poster that visually displays the four life cycles. 2) Use your notes, RQs, video notes and a computer or phone to complete the following: a) Name of star stage b) Color ...
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a large poster that visually displays the four life cycles. 2) Use your notes, RQs, video notes and a computer or phone to complete the following: a) Name of star stage b) Color ...
Chapter 1 Vocabulary – The Puzzled of Matter
... Nebula – a large cloud of gas and dust spread out over a large volume of space Protostar – a contracting nebula with enough mass to form a star Planetary Nebula – a glowing cloud of gas surrounding a dying low-mass star Supernova – an enormous explosion in which the byproducts of a supergiant star’s ...
... Nebula – a large cloud of gas and dust spread out over a large volume of space Protostar – a contracting nebula with enough mass to form a star Planetary Nebula – a glowing cloud of gas surrounding a dying low-mass star Supernova – an enormous explosion in which the byproducts of a supergiant star’s ...
Review Game
... areas of the corona where magnetic field lines project into space, allowing charged particles to escape the Sun, becoming the solar wind main sequence turnoff. by converting hydrogen to helium. the bubbling pattern on the photosphere produced by the underlying convection There is a balance within th ...
... areas of the corona where magnetic field lines project into space, allowing charged particles to escape the Sun, becoming the solar wind main sequence turnoff. by converting hydrogen to helium. the bubbling pattern on the photosphere produced by the underlying convection There is a balance within th ...
LIfe of a Star
... Used to study the lives of stars Most stars lie along the main sequence portion of the diagram ...
... Used to study the lives of stars Most stars lie along the main sequence portion of the diagram ...
fall semester review
... 34. Why is the Sun so bright in our sky during the day? It’s the closest star to earth and we are facing the sun during the ...
... 34. Why is the Sun so bright in our sky during the day? It’s the closest star to earth and we are facing the sun during the ...
Joining the Party - Lincoln-Sudbury Regional High School
... The evidence is the existence of T-Tauri stars: stars of 0.2 to 2 solar masses embedded in small dark molecular clouds. These stars have not yet quite reached the main sequence, but they are getting there. At least, we suspect so: these small stars evolve so slowly that we won’t be around long enoug ...
... The evidence is the existence of T-Tauri stars: stars of 0.2 to 2 solar masses embedded in small dark molecular clouds. These stars have not yet quite reached the main sequence, but they are getting there. At least, we suspect so: these small stars evolve so slowly that we won’t be around long enoug ...
Open clusters
... Review from last time: from observations of nearby stars, we can determine: distance to star apparent brightness luminosity spectral type temperature (for binary systems: mass) radius ...
... Review from last time: from observations of nearby stars, we can determine: distance to star apparent brightness luminosity spectral type temperature (for binary systems: mass) radius ...
Unit 12 Guide: Concepts of Earth Science Stars, Galaxies, and the
... 5. What is the difference between absolute and apparent magnitude? What is luminosity? 6. What are the three types of spectra? How can scientists use absorption spectra to determine the elements that compose a star? 7. What are stars made of and how do they produce their light? What is the differenc ...
... 5. What is the difference between absolute and apparent magnitude? What is luminosity? 6. What are the three types of spectra? How can scientists use absorption spectra to determine the elements that compose a star? 7. What are stars made of and how do they produce their light? What is the differenc ...
The Science behind the Stars ctY Astrophysics by Spencer McClung
... To put things simply, four hydrogen atoms under extremely immense pressure and temperature join to form a helium atom. Some of the mass of the hydrogen atoms is released as energy (as Mr. Einstein’s e=mc2 explains) when they form the lighter helium atom. This process repeats itself in the center of ...
... To put things simply, four hydrogen atoms under extremely immense pressure and temperature join to form a helium atom. Some of the mass of the hydrogen atoms is released as energy (as Mr. Einstein’s e=mc2 explains) when they form the lighter helium atom. This process repeats itself in the center of ...
Lifecycle of the stars.
... Small proto star-a brown dwarf that was too small to generate enough heat to start fusion. ...
... Small proto star-a brown dwarf that was too small to generate enough heat to start fusion. ...
HW #5 Answers (Due 9/29)
... 5. In a star cluster it is possible to tell how old the cluster is by looking at the mass of the stars that are just leaving the main sequence. Explain how this turn-off mass gives us the age of the cluster. As we found out in class, the more massive a star is the faster it uses up its fuel supply. ...
... 5. In a star cluster it is possible to tell how old the cluster is by looking at the mass of the stars that are just leaving the main sequence. Explain how this turn-off mass gives us the age of the cluster. As we found out in class, the more massive a star is the faster it uses up its fuel supply. ...
Study Guide - Universe Exam key 2014-15 v2
... c) How are color and temperature related? Red to blue = cooler to hotter d) How is luminosity and temperature related in the Main Sequence stars? They are equal e) In what two ways are the stars Sirius B and Regulus alike? Similar in temperature ...
... c) How are color and temperature related? Red to blue = cooler to hotter d) How is luminosity and temperature related in the Main Sequence stars? They are equal e) In what two ways are the stars Sirius B and Regulus alike? Similar in temperature ...
4. Star formation 4.1 Jeans` criterion
... which controls loss of radiation from surface. • Hence gravitational energy is radiated away on a thermal (Kelvin) timescale, tK~107 – 108 y. • Star remains close to hydrostatic equilibrium so we can continue to use Virial theorem. AS 3003 ...
... which controls loss of radiation from surface. • Hence gravitational energy is radiated away on a thermal (Kelvin) timescale, tK~107 – 108 y. • Star remains close to hydrostatic equilibrium so we can continue to use Virial theorem. AS 3003 ...
I Cloudy with a Chance of Making a star is no easy thing
... at a wavelength of 158 microns. Earth’s lower atmosphere is opaque at these wavelengths, so they must be observed using space-based observatories such as Herschel Space Observatory, launched last year by the European Space Agency, or telescopes mounted in airplanes, such as the Stratospheric Observa ...
... at a wavelength of 158 microns. Earth’s lower atmosphere is opaque at these wavelengths, so they must be observed using space-based observatories such as Herschel Space Observatory, launched last year by the European Space Agency, or telescopes mounted in airplanes, such as the Stratospheric Observa ...
Collapse: Method 2
... Stage 4. The high thermal pressure resists gravity and this ends the first collapse, forming what is traditionally called the first core at a density of 1013 cm-3 - 1014 cm-3 and temperature of 100-200 K. Stage 5. A shock wave forms at the outer edge of the first core. The first core accretes from t ...
... Stage 4. The high thermal pressure resists gravity and this ends the first collapse, forming what is traditionally called the first core at a density of 1013 cm-3 - 1014 cm-3 and temperature of 100-200 K. Stage 5. A shock wave forms at the outer edge of the first core. The first core accretes from t ...
File - Mr. Goodyear Astronomy
... proton-proton cycle. 90% of stars are main sequence stage. Stars are said to be in Hydrostatic Equilibrium: energy output = gravitational pull inward (known as hydrogen burning stage) - Stars like our sun last 10 billion years as a main sequence - ZAMS – zero age main sequence ...
... proton-proton cycle. 90% of stars are main sequence stage. Stars are said to be in Hydrostatic Equilibrium: energy output = gravitational pull inward (known as hydrogen burning stage) - Stars like our sun last 10 billion years as a main sequence - ZAMS – zero age main sequence ...
4. Star Formation
... at densities above 107 cm−3 the ionisation fraction is constant. For typical molecular cloud parameters the ambipolar diffusion timescale is about 10 – 20 times longer than the free fall time. These consideration lead to the investigation of star formation models based on ambipolar diffusion as a do ...
... at densities above 107 cm−3 the ionisation fraction is constant. For typical molecular cloud parameters the ambipolar diffusion timescale is about 10 – 20 times longer than the free fall time. These consideration lead to the investigation of star formation models based on ambipolar diffusion as a do ...
Ch. 11 and 12 Study Guide (ANSWERS)
... 15) What is a nebula (pg. 519)? A nebula is a cloud of dust and gas in space. 16) The elements, hydrogen and helium, are the most common in nebulae. 17) What is nuclear fusion? Nuclear fusion is a reaction in which 2 atomic nuclei combine to form a large nucleus with a higher mass. Energy is release ...
... 15) What is a nebula (pg. 519)? A nebula is a cloud of dust and gas in space. 16) The elements, hydrogen and helium, are the most common in nebulae. 17) What is nuclear fusion? Nuclear fusion is a reaction in which 2 atomic nuclei combine to form a large nucleus with a higher mass. Energy is release ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.