ppt
... How can we test theories of star evolution? • Binaries help, because one can get mass so that theories can be tested • But stars change so slowly, it is impossible to test theories by watching just one star move through phases • Fortunately, there are 1011 stars in our Galaxy, all with a range of ma ...
... How can we test theories of star evolution? • Binaries help, because one can get mass so that theories can be tested • But stars change so slowly, it is impossible to test theories by watching just one star move through phases • Fortunately, there are 1011 stars in our Galaxy, all with a range of ma ...
GEARS Workshop Monday - Georgia Southern University
... • Astronomers want nothing more than to classify and categorize – just like every other scientist • First thing we do is try to plot things on graphs to see if there is a pattern • Let’s plot two intrinsic properties against one another. ...
... • Astronomers want nothing more than to classify and categorize – just like every other scientist • First thing we do is try to plot things on graphs to see if there is a pattern • Let’s plot two intrinsic properties against one another. ...
14.5 Yellow Giants and Pulsating Stars Variable Stars Not all stars
... When a lowmass star crosses the region of the instability strip during its evolution as a red giant, it becomes an RR Lyrae variable star. When a highmass star crosses the instability strip in its red giant phase, being more luminous it instead becomes a Cepheid variable. The amount of time a give ...
... When a lowmass star crosses the region of the instability strip during its evolution as a red giant, it becomes an RR Lyrae variable star. When a highmass star crosses the instability strip in its red giant phase, being more luminous it instead becomes a Cepheid variable. The amount of time a give ...
Stellar Evolution - Academic Computer Center
... • Once neutrons are formed the collapse stops, the surrounding gas is heated and explodes off the core. This is a supernova explosion. • The explosion is so energetic that it can outshine the combined light of a galaxy! • Heavy elements are formed in the material blown off the star. These elements a ...
... • Once neutrons are formed the collapse stops, the surrounding gas is heated and explodes off the core. This is a supernova explosion. • The explosion is so energetic that it can outshine the combined light of a galaxy! • Heavy elements are formed in the material blown off the star. These elements a ...
Charcteristic of Stars Powerpoint C
... Characteristics of Stars Analyze how stars are classified based on their physical characteristics. ...
... Characteristics of Stars Analyze how stars are classified based on their physical characteristics. ...
Galaxy1
... • This means if we increased the volume that we are using to search for stars, we would start to bring in a few high mass stars, but the number of low mass stars would skyrocket. • Most stars in the Galaxy are low-mass, red dwarfs. ~90% of all stars. ...
... • This means if we increased the volume that we are using to search for stars, we would start to bring in a few high mass stars, but the number of low mass stars would skyrocket. • Most stars in the Galaxy are low-mass, red dwarfs. ~90% of all stars. ...
Ch. 15 Notes
... of light. This means that any object that gets too close would not be able to escape. • The existence of black holes was first proposed by Albert Einstein as a result of his Theory of General Relativity. He called them “dark stars”, but suggested these monsters could not possibly exist for real. • T ...
... of light. This means that any object that gets too close would not be able to escape. • The existence of black holes was first proposed by Albert Einstein as a result of his Theory of General Relativity. He called them “dark stars”, but suggested these monsters could not possibly exist for real. • T ...
Measuring the Distances to the Stars: Parallax What sets the parallax limit?
... • change in luminosity ...
... • change in luminosity ...
Project 8 : Stellar Spectra: Classification
... Absorption lines occur when an electron absorbs energy from the spectrum to move up the energy levels in the atom. Since hydrogen has only one electron, this electron is usually in the ground state. But as the temperature rises, the average electron gains m ...
... Absorption lines occur when an electron absorbs energy from the spectrum to move up the energy levels in the atom. Since hydrogen has only one electron, this electron is usually in the ground state. But as the temperature rises, the average electron gains m ...
Stars (Ch. 13)
... • To understand the properties of stars astronomers gathered hundreds of thousands of stellar spectra. • To understand the patterns they saw they developed spectral classification systems in order to help understand the nature of stars. • The first system was developed in 1866 by Pietro Angelo Secch ...
... • To understand the properties of stars astronomers gathered hundreds of thousands of stellar spectra. • To understand the patterns they saw they developed spectral classification systems in order to help understand the nature of stars. • The first system was developed in 1866 by Pietro Angelo Secch ...
Star- large ball of gas held together by large ball of gas held
... When the clump reaches the size of Jupiter, it creates enough energy by nuclear fusion to shine – becoming a star. For stars that are about the size of our sun, after main sequence they become giants, white dwarfs, and then black dwarfs. For stars larger than our sun, after main sequence and giant s ...
... When the clump reaches the size of Jupiter, it creates enough energy by nuclear fusion to shine – becoming a star. For stars that are about the size of our sun, after main sequence they become giants, white dwarfs, and then black dwarfs. For stars larger than our sun, after main sequence and giant s ...
HR Diagram Explorer Worksheet
... Open the HR Diagram Explorer. Begin by familiarizing yourself with the capabilities of the HertzsprungRussell Diagram Explorer through experimentation. An actual HR Diagram is provided in the upper right panel with an active location indicated by a red x. This active location can be dragged around ...
... Open the HR Diagram Explorer. Begin by familiarizing yourself with the capabilities of the HertzsprungRussell Diagram Explorer through experimentation. An actual HR Diagram is provided in the upper right panel with an active location indicated by a red x. This active location can be dragged around ...
Document
... Fate of planetary nebulae • Release the envelope into the ISM, on a timescale of ~10000 years. • There are probably about 15,000 in the Milky Way today ISM is being enriched at a rate of about 1 Msun/year. ...
... Fate of planetary nebulae • Release the envelope into the ISM, on a timescale of ~10000 years. • There are probably about 15,000 in the Milky Way today ISM is being enriched at a rate of about 1 Msun/year. ...
Topic 3 Assignment - Science 9 Portfolio
... The significance of the spectral lines was discovered about 50 years later when Kirschoff and Bunsen, two chemists used a spectroscope to observe various chemicals when they were heated. They found some of the lines missing in some of the chemicals. Each particular element had its own unique spectra ...
... The significance of the spectral lines was discovered about 50 years later when Kirschoff and Bunsen, two chemists used a spectroscope to observe various chemicals when they were heated. They found some of the lines missing in some of the chemicals. Each particular element had its own unique spectra ...
ASTR100 Class 01 - University of Maryland Department of
... What would happen to a protostar that formed without any rotation at all? A. Its jets would go in multiple directions. B. It would not have planets. C. It would be very bright in the infrared. D. It would not be round. ...
... What would happen to a protostar that formed without any rotation at all? A. Its jets would go in multiple directions. B. It would not have planets. C. It would be very bright in the infrared. D. It would not be round. ...
Part 1
... atop one another so the background stars (circles) line up. There are two nearby stars also shown. Which of these nearby stars is closer? ...
... atop one another so the background stars (circles) line up. There are two nearby stars also shown. Which of these nearby stars is closer? ...
MT 2 Answers Version C
... Choose the answer that best completes the question. Read each problem carefully and read through all the answers. Take your time. If a question is unclear, ask for clarification during the exam. Mark your answers on the scantron sheet and on your copy of the exam. Keep your copy of the exam and chec ...
... Choose the answer that best completes the question. Read each problem carefully and read through all the answers. Take your time. If a question is unclear, ask for clarification during the exam. Mark your answers on the scantron sheet and on your copy of the exam. Keep your copy of the exam and chec ...
te acher`s guide te acher`s guide
... Stars asks the following five questions about our Sun and all of its shining counterparts. Space travelers Adi and Woops help viewers clearly answer each question using computer graphics and space footage. What are the signs of the zodiac? The signs of the zodiac are twelve different groups of stars ...
... Stars asks the following five questions about our Sun and all of its shining counterparts. Space travelers Adi and Woops help viewers clearly answer each question using computer graphics and space footage. What are the signs of the zodiac? The signs of the zodiac are twelve different groups of stars ...
Surveys of Stars, The interstellar medium
... The Hertzsprung-Russell Diagram The HR diagram separates The effects of temperature And surface area on stars’ Luminosity and sorts the Stars according to their size ...
... The Hertzsprung-Russell Diagram The HR diagram separates The effects of temperature And surface area on stars’ Luminosity and sorts the Stars according to their size ...
Astro 3 Spring, 2004 (Prof
... The mass of a star determines its lifetime. High mass stars live short lives, while low mass stars live a long time. This is due to the fact that high mass stars burn their hydrogen much more quickly and efficiently than low mass stars. Some characteristic lifetimes are as follows: -- O Stars live ~ ...
... The mass of a star determines its lifetime. High mass stars live short lives, while low mass stars live a long time. This is due to the fact that high mass stars burn their hydrogen much more quickly and efficiently than low mass stars. Some characteristic lifetimes are as follows: -- O Stars live ~ ...
Evolution Cycle of Stars
... White Dwarf • This is very small, hot star, the last stage in the life cycle of a star like the Sun. • White dwarfs have a mass similar to that of the Sun, but only 1% of the Sun's diameter; approximately the diameter of the Earth. The surface temperature of a white dwarf is 8000C or more, but bein ...
... White Dwarf • This is very small, hot star, the last stage in the life cycle of a star like the Sun. • White dwarfs have a mass similar to that of the Sun, but only 1% of the Sun's diameter; approximately the diameter of the Earth. The surface temperature of a white dwarf is 8000C or more, but bein ...
The Life Cycle of a Star and the Hertzsprung
... great tool to check your understanding of the star life cycle. In the Hertzsprung-Russell (HR) Diagram, each star is represented by a dot. There are lots of stars out there, so there are lots of dots. The position of each dot on the diagram tells us two things about each star: its luminosity (bright ...
... great tool to check your understanding of the star life cycle. In the Hertzsprung-Russell (HR) Diagram, each star is represented by a dot. There are lots of stars out there, so there are lots of dots. The position of each dot on the diagram tells us two things about each star: its luminosity (bright ...
Stellar classification
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Light from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with absorption lines. Each line indicates an ion of a certain chemical element, with the line strength indicating the abundance of that ion. The relative abundance of the different ions varies with the temperature of the photosphere. The spectral class of a star is a short code summarizing the ionization state, giving an objective measure of the photosphere's temperature and density.Most stars are currently classified under the Morgan–Keenan (MK) system using the letters O, B, A, F, G, K, and M, a sequence from the hottest (O type) to the coolest (M type). Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest (e.g. A8, A9, F0, F1 form a sequence from hotter to cooler). The sequence has been expanded with classes for other stars and star-like objects that do not fit in the classical system, such class D for white dwarfs and class C for carbon stars.In the MK system a luminosity class is added to the spectral class using Roman numerals. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class 0 or Ia+ stars for hypergiants, class I stars for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main-sequence stars, class sd for sub-dwarfs, and class D for white dwarfs. The full spectral class for the Sun is then G2V, indicating a main-sequence star with a temperature around 5,800K.