Observations and Theoretical Models of Subdwarfs
... (2a) Distinguishing Features and Currently Understood Physical Model Cool subdwarfs are believed to be ancient stars which formed in the early stages of the formation of the Milky Way. Due to their early formation, the gas clouds from which these stars formed had been only slightly enriched with hea ...
... (2a) Distinguishing Features and Currently Understood Physical Model Cool subdwarfs are believed to be ancient stars which formed in the early stages of the formation of the Milky Way. Due to their early formation, the gas clouds from which these stars formed had been only slightly enriched with hea ...
Star Birth
... – Molecular H is hard to detect, since they do not emit light (radiation) – However, carbon monoxide present in these clouds emit millimeter wavelength light, and thus can be detected by radio telescopes. – these giant clouds have masses ranging from 105 - 106M. ...
... – Molecular H is hard to detect, since they do not emit light (radiation) – However, carbon monoxide present in these clouds emit millimeter wavelength light, and thus can be detected by radio telescopes. – these giant clouds have masses ranging from 105 - 106M. ...
Binary Star - Armagh Observatory
... You see gravity at work any time you drop a book, step on a scale or toss a ball up into the air. It's such a constant presence in our lives, we seldom marvel at the mystery of it but even with several well-received theories out there attempting to explain why a book falls to the ground (and at th ...
... You see gravity at work any time you drop a book, step on a scale or toss a ball up into the air. It's such a constant presence in our lives, we seldom marvel at the mystery of it but even with several well-received theories out there attempting to explain why a book falls to the ground (and at th ...
ASTR 1120 General Astronomy: Stars and Galaxies
... x-ray photon at 100A than the infrared light photons emitted by every living human? (Assuming 10,000nm wavelength of infrared light). • A. Ten times as powerful. • B. A hundred times more powerful. • C. A thousand times more powerful. • D. 1x1012 (a trillion) times more powerful. • E. 1x1015 (a quad ...
... x-ray photon at 100A than the infrared light photons emitted by every living human? (Assuming 10,000nm wavelength of infrared light). • A. Ten times as powerful. • B. A hundred times more powerful. • C. A thousand times more powerful. • D. 1x1012 (a trillion) times more powerful. • E. 1x1015 (a quad ...
The Sun and other Stars
... The amount of He is also increasing until H is expended and is no longer the fuel source for the star. He begins to fuse together. The star begins to be a pulsating Yellow Giant. The Star is extremely large and bright. Once the He is gone the star remains large but glows a cooler red. Becomi ...
... The amount of He is also increasing until H is expended and is no longer the fuel source for the star. He begins to fuse together. The star begins to be a pulsating Yellow Giant. The Star is extremely large and bright. Once the He is gone the star remains large but glows a cooler red. Becomi ...
Bright versus Nearby Stars
... Absolute Magnitudes of 269 Bright Stars • 95% of the brightest stars are more luminous than the Sun. • The average absolute magnitude of a bright star is –1.2, equivalent to 300 solar luminosities. ...
... Absolute Magnitudes of 269 Bright Stars • 95% of the brightest stars are more luminous than the Sun. • The average absolute magnitude of a bright star is –1.2, equivalent to 300 solar luminosities. ...
Carolina Kehrig
... explanation for the non-detection of WR features in some galaxy spectra Nearby narrow HeII emitters, specially metal-poor ones, are fundamental to better constrain models for metal-poor massive stars and understand high-z HeII emitters IFS of IZw18: reveal for the first time its total HeII-ioniz ...
... explanation for the non-detection of WR features in some galaxy spectra Nearby narrow HeII emitters, specially metal-poor ones, are fundamental to better constrain models for metal-poor massive stars and understand high-z HeII emitters IFS of IZw18: reveal for the first time its total HeII-ioniz ...
stars-notes
... Composition of Stars, continued • A continuous spectrum shows all of the colors, while an absorption spectrum shows which wavelengths of light are absorbed. • The spectrum of a star is an absorption spectrum because the atmosphere of the star absorbs certain portions of the light produced by the sta ...
... Composition of Stars, continued • A continuous spectrum shows all of the colors, while an absorption spectrum shows which wavelengths of light are absorbed. • The spectrum of a star is an absorption spectrum because the atmosphere of the star absorbs certain portions of the light produced by the sta ...
ASTR-1020: Astronomy II Course Lecture Notes Section III
... a) Thick lines: smaller stars, higher surface gravity. b) ...
... a) Thick lines: smaller stars, higher surface gravity. b) ...
STUDY GUIDE:
... The sun is a star! In fact, it is the closest star to earth, only 150 million kilometers (93 million miles) away. This may seem like a long way, but it’s still 250,000 times closer to us than the next closest star, which is Proxima Centauri. The sun is 4.6 billion years old and its light only takes ...
... The sun is a star! In fact, it is the closest star to earth, only 150 million kilometers (93 million miles) away. This may seem like a long way, but it’s still 250,000 times closer to us than the next closest star, which is Proxima Centauri. The sun is 4.6 billion years old and its light only takes ...
Brock physics - Brock University
... (d) [It depends on the whims of the head office of ProtoStar Inc.] 11. A brown dwarf is (a) a character in the Disney movie Snow White and the Dwarf Stars. (b) a white dwarf that has cooled near the end of its life. (c) a red dwarf that has cooled near the end of its life. (d) * a protostar that nev ...
... (d) [It depends on the whims of the head office of ProtoStar Inc.] 11. A brown dwarf is (a) a character in the Disney movie Snow White and the Dwarf Stars. (b) a white dwarf that has cooled near the end of its life. (c) a red dwarf that has cooled near the end of its life. (d) * a protostar that nev ...
10438 starlight - The Described and Captioned Media Program
... In this program, viewers examine how our basic knowledge about stars has been gained from studying the light we receive from stars. The study of starlight not only reveals straightforward information like the varying brightness of stars, but it also shows other details, such as their spectra, intens ...
... In this program, viewers examine how our basic knowledge about stars has been gained from studying the light we receive from stars. The study of starlight not only reveals straightforward information like the varying brightness of stars, but it also shows other details, such as their spectra, intens ...
Universe and Star Formation - White Plains Public Schools
... in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. ...
... in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. ...
2900 K micrometers T
... EMISSION lines in the hydrogen comparison spectrum). Other stars have additional elements too, because they have more absorption lines that are not accounted for by hydrogen. ...
... EMISSION lines in the hydrogen comparison spectrum). Other stars have additional elements too, because they have more absorption lines that are not accounted for by hydrogen. ...
talk / PPT / 1.6 MB
... Milky Way compared to External discs Where does the Milky Way lie on the ...
... Milky Way compared to External discs Where does the Milky Way lie on the ...
STEM for TY Teachers
... energy as the Sun is expected to emit over its entire life span. The explosion expels much or all of a star's material at a velocity of up to 30,000!km/s (10% of the speed of light), driving a shock wave into the surrounding interstellar medium. This shock wave produces an expanding shell of gas and ...
... energy as the Sun is expected to emit over its entire life span. The explosion expels much or all of a star's material at a velocity of up to 30,000!km/s (10% of the speed of light), driving a shock wave into the surrounding interstellar medium. This shock wave produces an expanding shell of gas and ...
Stars
... • For all Main Sequence stars, as surface temperature starts to increase, luminosity increases also _________________ • Most stars spend the majority of their life as Main Sequence stars ...
... • For all Main Sequence stars, as surface temperature starts to increase, luminosity increases also _________________ • Most stars spend the majority of their life as Main Sequence stars ...
After the ZAMS - Lincoln-Sudbury Regional High School
... The Big Ones Very massive stars evolve very quickly, in stellar terms, and so we can see a lot of these at different ages and stages. Remember too about look-back time: the further away a star is, the longer its light takes to reach us. So our cameras may be receiving light (and therefore images) w ...
... The Big Ones Very massive stars evolve very quickly, in stellar terms, and so we can see a lot of these at different ages and stages. Remember too about look-back time: the further away a star is, the longer its light takes to reach us. So our cameras may be receiving light (and therefore images) w ...
Star formation and lifetimes
... front of a red giant. 2. When an M spectral class main-sequence star is in front of a O spectral class main sequence star. 3. When a M spectral class main-sequence star is in front of a G spectral class star. 4. When a K spectral class main-sequence star is in front of a red giant. ...
... front of a red giant. 2. When an M spectral class main-sequence star is in front of a O spectral class main sequence star. 3. When a M spectral class main-sequence star is in front of a G spectral class star. 4. When a K spectral class main-sequence star is in front of a red giant. ...
Topic 3: The Spectroscope - Danielle`s science9 weebly
... 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 ...
Part A
... Beyond the convection zone are the three layers of a star’s atmosphere— the photosphere, the chromosphere, and the corona. ...
... Beyond the convection zone are the three layers of a star’s atmosphere— the photosphere, the chromosphere, and the corona. ...
How Old is the Universe?
... 95% confidence. They say the age is proportional to one over the luminosity of the RR Lyra stars which are used to determine the distances to globular clusters. Chaboyer (1997) gives a best estimate of 14.6 +/- 1.7 Gyr for the age of the globular clusters. But recent Hipparcos results show that the ...
... 95% confidence. They say the age is proportional to one over the luminosity of the RR Lyra stars which are used to determine the distances to globular clusters. Chaboyer (1997) gives a best estimate of 14.6 +/- 1.7 Gyr for the age of the globular clusters. But recent Hipparcos results show that the ...
Deriving the Isoradius Lines (optional, mathematical
... Uncheck show luminosity classes and check show instability strip. Note that this region of the HR Diagram indicates where pulsating stars are found such as RR Lyrae stars and Cepheid variable stars. These stars vary in brightness because they are pulsating – alternately growing bigger and smaller – ...
... Uncheck show luminosity classes and check show instability strip. Note that this region of the HR Diagram indicates where pulsating stars are found such as RR Lyrae stars and Cepheid variable stars. These stars vary in brightness because they are pulsating – alternately growing bigger and smaller – ...
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.