HR Diagram
... 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 – ...
Stars - Mike Brotherton
... Narrow absorption lines from Ca II: Too low ionization state and too narrow for the O star in the background; multiple components ...
... Narrow absorption lines from Ca II: Too low ionization state and too narrow for the O star in the background; multiple components ...
Lecture 8: The Stars - Department of Physics and Astronomy
... hydrogen from sea water, one gallon of seawater has the energy of 300 gallons of gasoline, 50 cups of water has energy of two tons of coal. ...
... hydrogen from sea water, one gallon of seawater has the energy of 300 gallons of gasoline, 50 cups of water has energy of two tons of coal. ...
Nature of Stars 2
... Observatory on the Draper Catalog, mapping and defining all the stars in the sky to photographic magnitude of about 9. Her Henry Draper Catalogue listed nearly 230,000 stars was valued as the work of a single observer. At this time the women astronomers doing this groundbreaking work at Harvard Obse ...
... Observatory on the Draper Catalog, mapping and defining all the stars in the sky to photographic magnitude of about 9. Her Henry Draper Catalogue listed nearly 230,000 stars was valued as the work of a single observer. At this time the women astronomers doing this groundbreaking work at Harvard Obse ...
sachkov_2013 - Putting A Stars into Context
... spectra and strong globally organized magnetic fields. They often show remarkable variations of line strengths, light and magnetic field with periods ranging from a few days to many years. It is believed that this abnormal chemical composition is limited only to the outer stellar envelopes. Chemical ...
... spectra and strong globally organized magnetic fields. They often show remarkable variations of line strengths, light and magnetic field with periods ranging from a few days to many years. It is believed that this abnormal chemical composition is limited only to the outer stellar envelopes. Chemical ...
inaugural091112
... Curiosity? Principles? The most fundamental science. Energy Environments Driver for emergence of totally new concepts Driver for pioneering technology ...
... Curiosity? Principles? The most fundamental science. Energy Environments Driver for emergence of totally new concepts Driver for pioneering technology ...
Whiteq
... space, forming a nebula. The nebula is visible because it is heated by ionizing radiation, from the hot central star. They tend to appear as rings around the stars, but are really semi-transparent shells, that totally surround the stars. Most nebulae are less than 50,000 years old, which fits in wel ...
... space, forming a nebula. The nebula is visible because it is heated by ionizing radiation, from the hot central star. They tend to appear as rings around the stars, but are really semi-transparent shells, that totally surround the stars. Most nebulae are less than 50,000 years old, which fits in wel ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... The existence of a superwind is suggested by two independent variables. The high density observed within the observed shells in stellar ejecta, and relative paucity of very bright stars on the AGB. The latter (Prialnik P. 161) comes from the number of AGB stars expected compared to observed is >10. ...
... The existence of a superwind is suggested by two independent variables. The high density observed within the observed shells in stellar ejecta, and relative paucity of very bright stars on the AGB. The latter (Prialnik P. 161) comes from the number of AGB stars expected compared to observed is >10. ...
L10 - QUB Astrophysics Research Centre
... The existence of a superwind is suggested by two independent variables. The high density observed within the observed shells in stellar ejecta, and relative paucity of very bright stars on the AGB. The latter (Prialnik P. 161) comes from the number of AGB stars expected compared to observed is >10. ...
... The existence of a superwind is suggested by two independent variables. The high density observed within the observed shells in stellar ejecta, and relative paucity of very bright stars on the AGB. The latter (Prialnik P. 161) comes from the number of AGB stars expected compared to observed is >10. ...
The Birth, Life, and Death of Stars
... A protostar achieves stardom at 10 million K Gravitational energy converted into thermal/kinetic energy Protons overcome their Coulomb repulsion and fuse Thermonuclear energy is generated by converting 4 protons into 4 He What happens after H fuel is exhausted in the stellar core? Stars are remarkab ...
... A protostar achieves stardom at 10 million K Gravitational energy converted into thermal/kinetic energy Protons overcome their Coulomb repulsion and fuse Thermonuclear energy is generated by converting 4 protons into 4 He What happens after H fuel is exhausted in the stellar core? Stars are remarkab ...
key for the HR Diagram Lab Handout
... Geminorum have brightness of 9,000 Suns and 310 Suns respectively; these stars are much larger than Proxima and Barnard s with brightness of 0.00005 and 0.0003 Suns. The significant difference in brightness with no change in temperature means that Betelgeuse and Mu Geminorum are much larger than the ...
... Geminorum have brightness of 9,000 Suns and 310 Suns respectively; these stars are much larger than Proxima and Barnard s with brightness of 0.00005 and 0.0003 Suns. The significant difference in brightness with no change in temperature means that Betelgeuse and Mu Geminorum are much larger than the ...
Astronomy Webquest Part 1: Life of Stars: Go to http://www.odec.ca
... 3. Near the end of the main sequence, when there is not enough hydrogen gas to support the star, the outer layers will ______________ in an attempt to ______________________________. 4. This forms a ____________. Click on next. 5. After the core collapses due to lack of hydrogen, the red giant will ...
... 3. Near the end of the main sequence, when there is not enough hydrogen gas to support the star, the outer layers will ______________ in an attempt to ______________________________. 4. This forms a ____________. Click on next. 5. After the core collapses due to lack of hydrogen, the red giant will ...
Astronomy Final C - Tarleton State University
... 5. Degenerate gases ? cool without losing their pressure. A.can B.cannot 6. ? develop where supernova explosions leave behind a “core” of approximately 1.4 to 2 or 3 stellar masses. A.Brown Dwarfs B.Red Dwarfs C.White Dwarfs D.Neutron Stars E.Black Holes 7. Inertial Mass ? gravitational mass. A.equa ...
... 5. Degenerate gases ? cool without losing their pressure. A.can B.cannot 6. ? develop where supernova explosions leave behind a “core” of approximately 1.4 to 2 or 3 stellar masses. A.Brown Dwarfs B.Red Dwarfs C.White Dwarfs D.Neutron Stars E.Black Holes 7. Inertial Mass ? gravitational mass. A.equa ...
3P15.pdf
... have short duration flares that happen very frequently (Crespo-Chacón 2004a, b, c; Montes et al. 2004). Therefore, more than a flare could have taken place during the exposure time of our observations (see Table. 1). In fact, it can be clearly noticed that our flare stars are out of the tendency fol ...
... have short duration flares that happen very frequently (Crespo-Chacón 2004a, b, c; Montes et al. 2004). Therefore, more than a flare could have taken place during the exposure time of our observations (see Table. 1). In fact, it can be clearly noticed that our flare stars are out of the tendency fol ...
Astronomy Activity: The Life-Line of the Stars
... Just like a fire flame (like a burning match) has different colors, so do the stars. This is because stars have different temperatures. Really hot stars are blue or white-hot. Cool stars are red or redish-orange in color. Astronomers classify stars based on what they are made of (in addition to hydr ...
... Just like a fire flame (like a burning match) has different colors, so do the stars. This is because stars have different temperatures. Really hot stars are blue or white-hot. Cool stars are red or redish-orange in color. Astronomers classify stars based on what they are made of (in addition to hydr ...
THE PHYSICAL CHARACTERIZATION OF THE STARS 1
... gravitational collapse of giant and cold clouds of molecular gas, take long episodes of production of energy through thermonuclear reactions in their interior with a length that depends on the mass, and die as highly compact objects. The life of an isolated star is mainly driven by their initial mas ...
... gravitational collapse of giant and cold clouds of molecular gas, take long episodes of production of energy through thermonuclear reactions in their interior with a length that depends on the mass, and die as highly compact objects. The life of an isolated star is mainly driven by their initial mas ...
Photometric Surveys and Variable stars
... Gamma Doradus stars • sp. type mid-late F, lum. class V, Pop I • P: 8h - 3d (close to P(rot)!) • sometimes multiperiodic • g-mode pulsators (n < 0) The gamma Doradus class is a new designation (early 1990’s). Before they were discovered, they were sometimes unknowingly used as comp stars! ...
... Gamma Doradus stars • sp. type mid-late F, lum. class V, Pop I • P: 8h - 3d (close to P(rot)!) • sometimes multiperiodic • g-mode pulsators (n < 0) The gamma Doradus class is a new designation (early 1990’s). Before they were discovered, they were sometimes unknowingly used as comp stars! ...
Stellar Spectra
... A low-density gas excited to emit light will do so at specific wavelengths and thus produce an emission spectrum. ...
... A low-density gas excited to emit light will do so at specific wavelengths and thus produce an emission spectrum. ...
Wien`s Law and Temperature
... that were shown on the blackbody simulation. Fill in the table below for the temperature estimate for each star. If the peak wavelength is not on the spectra graph for the star, state whether it is on the infrared (IR) or the ultraviolet (UV) side of the spectrum. Use the temperature determined from ...
... that were shown on the blackbody simulation. Fill in the table below for the temperature estimate for each star. If the peak wavelength is not on the spectra graph for the star, state whether it is on the infrared (IR) or the ultraviolet (UV) side of the spectrum. Use the temperature determined from ...
Stars: Properties and Classification
... made of, what kinds are out there, how they are born, and how they die. Are all stars similar to our Sun? How far away are they? Where did they come from? What do they do? Do they live forever? How do they die? ...
... made of, what kinds are out there, how they are born, and how they die. Are all stars similar to our Sun? How far away are they? Where did they come from? What do they do? Do they live forever? How do they die? ...
NEUTRON STAR?
... • We will be holding an optional observing night this coming Tuesday, Nov. 8th from 7-9 p.m. on the Science Center roof. We'll be looking at Mars, stellar clusters, binary stars, and more... • Because we live in lovely cloudy Boston, we have to prepare for inclement weather. We will make an announce ...
... • We will be holding an optional observing night this coming Tuesday, Nov. 8th from 7-9 p.m. on the Science Center roof. We'll be looking at Mars, stellar clusters, binary stars, and more... • Because we live in lovely cloudy Boston, we have to prepare for inclement weather. We will make an announce ...
Solutions
... as luminous as an entire galaxy. However, they are very different sorts of objects. What is the original source of the energy which powers each type of explosion? (I.e. where did the energy come from that allowed the energy in the explosion to be released?) Type Ia: fusion of carbon to heavier eleme ...
... as luminous as an entire galaxy. However, they are very different sorts of objects. What is the original source of the energy which powers each type of explosion? (I.e. where did the energy come from that allowed the energy in the explosion to be released?) Type Ia: fusion of carbon to heavier eleme ...
Lecture 15 (pdf from the powerpoint)
... • Iron cannot be fused into any heavier element, so it collects at the center of the star • Gravity pulls the core of the star to a size smaller than the Earth’s diameter! • The core compresses so much that protons and electrons merge into neutrons, taking energy away from the core • The core collap ...
... • Iron cannot be fused into any heavier element, so it collects at the center of the star • Gravity pulls the core of the star to a size smaller than the Earth’s diameter! • The core compresses so much that protons and electrons merge into neutrons, taking energy away from the core • The core collap ...
Ch 28 Outline
... → particles of gas and dust move closer together due to gravity → become DENSER → temperature INCREASES → begins to glow (protostars). As contraction continues, protostars become HOTTER and BRIGHTER → nuclear fusion begins and the STAR IS BORN. Death of a Star Like the Sun These stars remain about t ...
... → particles of gas and dust move closer together due to gravity → become DENSER → temperature INCREASES → begins to glow (protostars). As contraction continues, protostars become HOTTER and BRIGHTER → nuclear fusion begins and the STAR IS BORN. Death of a Star Like the Sun These stars remain about t ...
ISM and star formation
... Regions of gas and dust near stars just formed. The Hydrogen is essentially fully ionized. Temperatures near 10,000 K Sizes about 1-20 pc. Hot tenuous gas => emission lines (Kirchhoff's Laws) ...
... Regions of gas and dust near stars just formed. The Hydrogen is essentially fully ionized. Temperatures near 10,000 K Sizes about 1-20 pc. Hot tenuous gas => emission lines (Kirchhoff's Laws) ...
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.