16. Properties of Stars
... Lifetime on the Main Sequence How long will it be before MS stars run out of fuel? i.e. Hydrogen? How much fuel is there? M How fast is it consumed? L M How long before it is used up? Time = Amount/(rate it is being used) ...
... Lifetime on the Main Sequence How long will it be before MS stars run out of fuel? i.e. Hydrogen? How much fuel is there? M How fast is it consumed? L M How long before it is used up? Time = Amount/(rate it is being used) ...
Star Properties and Stellar Evolution
... Stars are classified using surface temperature and absolute magnitude. ...
... Stars are classified using surface temperature and absolute magnitude. ...
Hertzsprung-Russell Diagram—key to understanding properties of stars. 26 Sept
... • The spectrum of the “A” star shows strong lines of hydrogen and weaker lines of many other elements. ...
... • The spectrum of the “A” star shows strong lines of hydrogen and weaker lines of many other elements. ...
Stars - Weebly
... Life Cycle of Stars • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the univ ...
... Life Cycle of Stars • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the univ ...
Star project
... • They are extremely burning hot. • The nearest star to us is the sun. • They are made up of mainly hydrogen and helium, but have a little bit of other elements like oxygen and carbon as well. ...
... • They are extremely burning hot. • The nearest star to us is the sun. • They are made up of mainly hydrogen and helium, but have a little bit of other elements like oxygen and carbon as well. ...
star
... brightness. Other important properties of stars include their chemical composition and mass. ...
... brightness. Other important properties of stars include their chemical composition and mass. ...
Life Cycle of Stars - Faulkes Telescope Project
... they spend the rest of their lives slowly leaking out energy that was formed during it’s nuclear fusion phases. ...
... they spend the rest of their lives slowly leaking out energy that was formed during it’s nuclear fusion phases. ...
The Hertzsprung-Russell Diagram
... Full classification of stars includes both spectral type and luminosity class: – Spectral type: OBAFGKM – Luminosity Class in descending order: • I: Supergiants • II: Bright giants • III: Giants • IV: Subgiants • V: Main-sequence stars – The full classification of a star includes both a spectral typ ...
... Full classification of stars includes both spectral type and luminosity class: – Spectral type: OBAFGKM – Luminosity Class in descending order: • I: Supergiants • II: Bright giants • III: Giants • IV: Subgiants • V: Main-sequence stars – The full classification of a star includes both a spectral typ ...
Stars
... Life Cycle of Stars • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the univ ...
... Life Cycle of Stars • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the univ ...
April 2005
... Application: Separate close Binary Stars • Too distant to resolve the individual stars • Can be viewed indirectly by observing the back-and-forth Doppler shifts of their spectral lines ...
... Application: Separate close Binary Stars • Too distant to resolve the individual stars • Can be viewed indirectly by observing the back-and-forth Doppler shifts of their spectral lines ...
So why are more massive stars more luminous?
... ability to form stars? •A) Star formation is so complicated that it is not possible to say how one quantity, such as temperature, affects it •B) Higher temperatures inhibit star formation •C) Higher temperatures help star formation •D) Star formation is independent of the temperature of the cloud ...
... ability to form stars? •A) Star formation is so complicated that it is not possible to say how one quantity, such as temperature, affects it •B) Higher temperatures inhibit star formation •C) Higher temperatures help star formation •D) Star formation is independent of the temperature of the cloud ...
Lecture21 - UCSB Physics
... ability to form stars? • A) Star formation is so complicated that it is not possible to say how one quantity, such as temperature, affects it • B) Higher temperatures inhibit star formation • C) Higher temperatures help star formation • D) Star formation is independent of the temperature of the clou ...
... ability to form stars? • A) Star formation is so complicated that it is not possible to say how one quantity, such as temperature, affects it • B) Higher temperatures inhibit star formation • C) Higher temperatures help star formation • D) Star formation is independent of the temperature of the clou ...
29.2 Measuring the Stars - Mr. Tobin`s Earth Science Class
... • Earth’s orbit around the Sun means that ...
... • Earth’s orbit around the Sun means that ...
Lecture 5
... Mass-Luminosity Relation for MainSequence Stars • Main sequence stars are stars like the Sun but with different masses • The mass-luminosity relation expresses a direct correlation between mass and luminosity for main-sequence stars • The greater the mass of a main-sequence star, the greater its lu ...
... Mass-Luminosity Relation for MainSequence Stars • Main sequence stars are stars like the Sun but with different masses • The mass-luminosity relation expresses a direct correlation between mass and luminosity for main-sequence stars • The greater the mass of a main-sequence star, the greater its lu ...
10 - Keele Astrophysics Group
... the continuum. By the end of that century, astronomers were able to examine the spectra of stars in large numbers and realised that stars could be divided into groups according to the general appearance of their spectra. Classification schemes were developed that grouped together stars depending on ...
... the continuum. By the end of that century, astronomers were able to examine the spectra of stars in large numbers and realised that stars could be divided into groups according to the general appearance of their spectra. Classification schemes were developed that grouped together stars depending on ...
STAR FORMATION (Ch. 19) The basics: GRAVITY vs. PRESSURE
... when stars can just balance gravity with pressure at all layers, and will spend about 90% of their lives in this stage. Different stellar masses: arrive at the main sequence at different temperatures and luminosities. See Fig. 19.8. Note: the “main sequence” is the location in the H-R diagram of all ...
... when stars can just balance gravity with pressure at all layers, and will spend about 90% of their lives in this stage. Different stellar masses: arrive at the main sequence at different temperatures and luminosities. See Fig. 19.8. Note: the “main sequence” is the location in the H-R diagram of all ...
Lecture 19 The Milky Way Galaxy
... • Romans called it ‘via lactia’ – milky road, or milky way • But what is it? • By the mid-18th century, astronomers new that it was made up of an enormous number of distant stars ...
... • Romans called it ‘via lactia’ – milky road, or milky way • But what is it? • By the mid-18th century, astronomers new that it was made up of an enormous number of distant stars ...
Star Stuff
... • where the electrons are located (which energy levels) • which elements have absorption, emission lines -- an O-star has a temperature of ~50,000 K -- an A-star has a temp of ~10,000 K, enough for hydrogen to be ionized (spectral lines in the UV) -- a G-star (like our Sun) has a temperature of ~6,0 ...
... • where the electrons are located (which energy levels) • which elements have absorption, emission lines -- an O-star has a temperature of ~50,000 K -- an A-star has a temp of ~10,000 K, enough for hydrogen to be ionized (spectral lines in the UV) -- a G-star (like our Sun) has a temperature of ~6,0 ...
WHERE DO WE SEARCH FOR LIFE IN THE UNIVERSE?
... Elimination of Low Mass Stars If we eliminate all stars that have a luminosity that is less than 1% of the Sun’s, then we eliminate nearly 75% of all stars in the Milky Way! ...
... Elimination of Low Mass Stars If we eliminate all stars that have a luminosity that is less than 1% of the Sun’s, then we eliminate nearly 75% of all stars in the Milky Way! ...
Document
... j. How is it possible that Canopus is more luminous than Achernar, given their respective spectral types? Canopus is cooler than Achernar; therefore, the only way Canopus can be more luminous is because it is LARGER. 2. List the evolutionary stages of the Sun’s life cycle & describe how its size (Ra ...
... j. How is it possible that Canopus is more luminous than Achernar, given their respective spectral types? Canopus is cooler than Achernar; therefore, the only way Canopus can be more luminous is because it is LARGER. 2. List the evolutionary stages of the Sun’s life cycle & describe how its size (Ra ...
PHYSICS 015
... For the most massive stars, the Schwarzschild radius is already too big. For example, if you wanted to allow a 10-solar-mass star to settle down as a neutron star, about 10 km in diameter, it already inside its Schwarzschild radius and is doomed to collapse! Stars can’t ‘know’ that they should shed ...
... For the most massive stars, the Schwarzschild radius is already too big. For example, if you wanted to allow a 10-solar-mass star to settle down as a neutron star, about 10 km in diameter, it already inside its Schwarzschild radius and is doomed to collapse! Stars can’t ‘know’ that they should shed ...
The Classification of Stellar Spectra
... Astronomers use one of several mnemonics to remember the order of the classification scheme. O, B, and A type stars are often referred to as early spectral types, while cool stars (G, K, and M) are known as late type stars. The nomenclature is rooted in long-obsolete ideas about stellar evolution, b ...
... Astronomers use one of several mnemonics to remember the order of the classification scheme. O, B, and A type stars are often referred to as early spectral types, while cool stars (G, K, and M) are known as late type stars. The nomenclature is rooted in long-obsolete ideas about stellar evolution, b ...
Solar Spectrum Birth of Spectroscopy Kirchhoff`s Laws Types of
... between luminosity and temperature using data from Cannon ...
... between luminosity and temperature using data from Cannon ...
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.