What is an atom?
... In the last chapter you read how telescopes gather light from the stars and how spectrographs spread the light out into spectra. Now you are ready to see what all the fuss is about. Spectra contain the secrets of the stars. Here you will find answers to four essential ...
... In the last chapter you read how telescopes gather light from the stars and how spectrographs spread the light out into spectra. Now you are ready to see what all the fuss is about. Spectra contain the secrets of the stars. Here you will find answers to four essential ...
Why is there a main sequence?
... Mmax ~ 100 solar masses a) More massive clouds fragment into smaller pieces during star formation ...
... Mmax ~ 100 solar masses a) More massive clouds fragment into smaller pieces during star formation ...
12.4 Evolution of Stars More Massive than the Sun
... It can be seen from this H-R diagram that stars more massive than the Sun follow very different paths when leaving the Main Sequence: ...
... It can be seen from this H-R diagram that stars more massive than the Sun follow very different paths when leaving the Main Sequence: ...
Exam2 Review Slides
... Photons have a difficult time moving through a star’s atmosphere If the photon has the right energy, it will be absorbed by an atom and raise an electron to a higher energy level Creates absorption spectra, a unique “fingerprint” for the star’s composition. The strength of this spectra is determined ...
... Photons have a difficult time moving through a star’s atmosphere If the photon has the right energy, it will be absorbed by an atom and raise an electron to a higher energy level Creates absorption spectra, a unique “fingerprint” for the star’s composition. The strength of this spectra is determined ...
The Electromagnetic Spectrum
... • What is an emission spectrum? • What is an absorption spectrum? • Why do we know that Hydrogen and Helium are found on most stars? • How do we know that the Sun’s surface temperature is 5800 °K? • What is the Doppler Effect? What does it tell us? • How would we name the fourth brightest star in th ...
... • What is an emission spectrum? • What is an absorption spectrum? • Why do we know that Hydrogen and Helium are found on most stars? • How do we know that the Sun’s surface temperature is 5800 °K? • What is the Doppler Effect? What does it tell us? • How would we name the fourth brightest star in th ...
File
... • The remaining dense core is made up almost entirely of neutrons. • This is called a neutron star. • These are as small as 10 miles across. • They are extremely dense. • 1 tsp. of neutron star matter = 1 billion tons • The Neutron star begins to spin rapidly and create a large magnetic field that b ...
... • The remaining dense core is made up almost entirely of neutrons. • This is called a neutron star. • These are as small as 10 miles across. • They are extremely dense. • 1 tsp. of neutron star matter = 1 billion tons • The Neutron star begins to spin rapidly and create a large magnetic field that b ...
Absolute magnitude
... largest hot plate. The temperatures of the hot plates are coded: the lighter the shade of gray, the higher the temperature. ...
... largest hot plate. The temperatures of the hot plates are coded: the lighter the shade of gray, the higher the temperature. ...
Lecture 13: The stars are suns
... is measured in watts per m2 . Flux from the Sun (at the Earth) = 1.4 kW/m2 . Flux from Sirius (at the Earth) = 1/107 W/m2 . Flux (Sun) = 10 billion x Flux (Sirius). • Historically astronomers measure the brightness of stars in magnitudes. Magnitude system was invented by Hipparchus (190-120 BC) – he ...
... is measured in watts per m2 . Flux from the Sun (at the Earth) = 1.4 kW/m2 . Flux from Sirius (at the Earth) = 1/107 W/m2 . Flux (Sun) = 10 billion x Flux (Sirius). • Historically astronomers measure the brightness of stars in magnitudes. Magnitude system was invented by Hipparchus (190-120 BC) – he ...
Lecture 37: The Pale Blue Dot
... Direct detection of exoEarths is hard because of their small size and extreme faintness relative to their parent stars. The spectrum of the Earth has two humps: reflected sunlight and thermal emission. Spectral properties can measure the size and surface temperatures of exoEarths. Spectral biomarker ...
... Direct detection of exoEarths is hard because of their small size and extreme faintness relative to their parent stars. The spectrum of the Earth has two humps: reflected sunlight and thermal emission. Spectral properties can measure the size and surface temperatures of exoEarths. Spectral biomarker ...
Lecture 19 Brightness Units
... Main Sequence 90% of stars. eg the Sun . The least luminous (coolest) main sequence stars are by far the most common (albeit the most inconspicuous) • White Dwarfs (a different typing scheme). Probably very common, but so faint that not many are known. eg Sirius B (faint companion to Sirius) Next ti ...
... Main Sequence 90% of stars. eg the Sun . The least luminous (coolest) main sequence stars are by far the most common (albeit the most inconspicuous) • White Dwarfs (a different typing scheme). Probably very common, but so faint that not many are known. eg Sirius B (faint companion to Sirius) Next ti ...
White Dwarf Stars - University of California Observatories
... • Neutron stars are stellar cores that are more massive than the Chandrasekhar limit (1.44 M☼). • They are held up against their own intense gravity by the tendency for neutrons to be incompressible (neutron degeneracy pressure). • Their gravity is too strong to be supported by electron degeneracy p ...
... • Neutron stars are stellar cores that are more massive than the Chandrasekhar limit (1.44 M☼). • They are held up against their own intense gravity by the tendency for neutrons to be incompressible (neutron degeneracy pressure). • Their gravity is too strong to be supported by electron degeneracy p ...
File - Mr. Goodyear Astronomy
... Spectral classification of stars - Stars are classified by the temperature and the element spectral lines found in the star. Classified by letters and numbers O B A F G K M “oh be a fine girl/guy kiss me” Each has 10 sub categories numbers from 0 to 9 ...
... Spectral classification of stars - Stars are classified by the temperature and the element spectral lines found in the star. Classified by letters and numbers O B A F G K M “oh be a fine girl/guy kiss me” Each has 10 sub categories numbers from 0 to 9 ...
Integrative Studies 410 Our Place in the Universe
... • increasing temperature at core slows contraction – Luminosity about 1000 times that of the sun – Duration ~ 1 million years – Temperature ~ 1 million K at core, 3,000 K at surface • Still too cool for nuclear fusion! ...
... • increasing temperature at core slows contraction – Luminosity about 1000 times that of the sun – Duration ~ 1 million years – Temperature ~ 1 million K at core, 3,000 K at surface • Still too cool for nuclear fusion! ...
Microsoft Power Point version
... Open clusters contain up to several thousand stars and are found in the disk of the galaxy. Globular clusters are much denser, containing hundreds of thousands of stars, and are found in both the halo and disk of the galaxy. Globular cluster stars are among the oldest stars known, with ages of about ...
... Open clusters contain up to several thousand stars and are found in the disk of the galaxy. Globular clusters are much denser, containing hundreds of thousands of stars, and are found in both the halo and disk of the galaxy. Globular cluster stars are among the oldest stars known, with ages of about ...
16. Properties of Stars
... Open clusters contain up to several thousand stars and are found in the disk of the galaxy. Globular clusters are much denser, containing hundreds of thousands of stars, and are found in both the halo and disk of the galaxy. Globular cluster stars are among the oldest stars known, with ages of about ...
... Open clusters contain up to several thousand stars and are found in the disk of the galaxy. Globular clusters are much denser, containing hundreds of thousands of stars, and are found in both the halo and disk of the galaxy. Globular cluster stars are among the oldest stars known, with ages of about ...
HERE
... habits. Orange, yellow or white in color. Typically will live for 1-20 billion years. Spectral class M,R,N, L stars: (most abundant): Small, cool, Red, and dim. Will burn the slowest and live the longest (about 50billion years). ...
... habits. Orange, yellow or white in color. Typically will live for 1-20 billion years. Spectral class M,R,N, L stars: (most abundant): Small, cool, Red, and dim. Will burn the slowest and live the longest (about 50billion years). ...
Slide 1 - Physics @ IUPUI
... • So it falls back, and will overshoot the other way going too far in • The process then continues ...
... • So it falls back, and will overshoot the other way going too far in • The process then continues ...
Section 1
... (cf. Appendix E), or spectral type. The ultimate goal is to relate these observationally accessible quantities to the physical parameters, and thence to make inferences about stellar structure and evolution. The spectrum is a particularly powerful tool in this endeavour, because, as already noted, t ...
... (cf. Appendix E), or spectral type. The ultimate goal is to relate these observationally accessible quantities to the physical parameters, and thence to make inferences about stellar structure and evolution. The spectrum is a particularly powerful tool in this endeavour, because, as already noted, t ...
Universe Notes - Solon City Schools
... an H-R diagram where most stars spend 90% of their life. i. A diagonal band running from the bright, hot stars on the upper left to the dim, cool stars on the lower right ii. Example: The Sun lies in the main sequence ...
... an H-R diagram where most stars spend 90% of their life. i. A diagonal band running from the bright, hot stars on the upper left to the dim, cool stars on the lower right ii. Example: The Sun lies in the main sequence ...
Stars - Moodle
... • Astronomers analyze stars by looking at the light they emit • They use a spectrograph • A spectrograph separates light into different colors or wavelengths • Stars produce a display of colors and lines called a spectrum ...
... • Astronomers analyze stars by looking at the light they emit • They use a spectrograph • A spectrograph separates light into different colors or wavelengths • Stars produce a display of colors and lines called a spectrum ...
Stars, Stellar classification, H
... hydrogenburning stars reside on the main sequence of the H-R ...
... hydrogenburning stars reside on the main sequence of the H-R ...
absolute magnitude
... The Key Tool to understanding Stars: the Hertzsprung-Russell diagram • Hertzsprung-Russell diagram is luminosity vs. spectral type (or temperature) • To obtain a HR diagram: – get the luminosity. This is your y-coordinate. – Then take the spectral type as your x-coordinate, e.g. K5 for Aldebaran. F ...
... The Key Tool to understanding Stars: the Hertzsprung-Russell diagram • Hertzsprung-Russell diagram is luminosity vs. spectral type (or temperature) • To obtain a HR diagram: – get the luminosity. This is your y-coordinate. – Then take the spectral type as your x-coordinate, e.g. K5 for Aldebaran. F ...
Surveying the Stars
... luminosities. • Read about apparent magnitudes here, and absolute magnitude here, as well as in the text. We don’t have time in the course to get more mathematical than this ...
... luminosities. • Read about apparent magnitudes here, and absolute magnitude here, as well as in the text. We don’t have time in the course to get more mathematical than this ...
HR DIAGRAM REPORT FORM
... Using the enclosed graph sheets and the background handout, complete the following plots. Graphs – 10 pts each Questions – 3 pts each A. Plot an H-R diagram for the brightest stars from table 10.1. B. Plot an H-R diagram for the closest stars from table 10.2. 1. Which type of star is most common on ...
... Using the enclosed graph sheets and the background handout, complete the following plots. Graphs – 10 pts each Questions – 3 pts each A. Plot an H-R diagram for the brightest stars from table 10.1. B. Plot an H-R diagram for the closest stars from table 10.2. 1. Which type of star is most common on ...
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.