The resolved stellar populations of M32 Monachesi, Antonela
... we can reconstruct the history of a galaxy from its constituent stars. Stars have imprinted in their properties information about the chemical composition of the intergalactic gas from where they formed, and also about their ages. The radiation emitted by a star is produced in its interior and relea ...
... we can reconstruct the history of a galaxy from its constituent stars. Stars have imprinted in their properties information about the chemical composition of the intergalactic gas from where they formed, and also about their ages. The radiation emitted by a star is produced in its interior and relea ...
CS3_Ch 3 - Leon County Schools
... • Astronomers learn about the energy, distance, temperature, and composition of stars by studying their light. • Astronomers measure distances in space in astrological units and in light-years. They measure star brightness as apparent magnitude and as luminosity. ...
... • Astronomers learn about the energy, distance, temperature, and composition of stars by studying their light. • Astronomers measure distances in space in astrological units and in light-years. They measure star brightness as apparent magnitude and as luminosity. ...
Chapter 26.2 notes
... The Hertzsprung-Russell Diagram Giants and Dwarfs In general, two factors determine a star’s absolute brightness: its size and its surface temperature. An H-R diagram shows a star’s absolute brightness and surface temperature. • If you compare two stars at the same temperature, the brighter one must ...
... The Hertzsprung-Russell Diagram Giants and Dwarfs In general, two factors determine a star’s absolute brightness: its size and its surface temperature. An H-R diagram shows a star’s absolute brightness and surface temperature. • If you compare two stars at the same temperature, the brighter one must ...
Stars and Galaxies - La Salle Elementary Public Schools No 122
... • Astronomers learn about the energy, distance, temperature, and composition of stars by studying their light. • Astronomers measure distances in space in astrological units and in light-years. They measure star brightness as apparent magnitude and as luminosity. ...
... • Astronomers learn about the energy, distance, temperature, and composition of stars by studying their light. • Astronomers measure distances in space in astrological units and in light-years. They measure star brightness as apparent magnitude and as luminosity. ...
Studying Variable stars using Small Telescopes Observational
... Lunar and Planetary Occultation ...
... Lunar and Planetary Occultation ...
Star Clusters and their stars
... In globular clusters, no new stars have been formed after the original episode of star formation – the gas was blown out of the cluster because of star light. Therefore, the brightest (shorterlived) stars have left the main sequence. Cluster age can be determined from the brightest stars still in th ...
... In globular clusters, no new stars have been formed after the original episode of star formation – the gas was blown out of the cluster because of star light. Therefore, the brightest (shorterlived) stars have left the main sequence. Cluster age can be determined from the brightest stars still in th ...
Star_Clusters
... In globular clusters, no new stars have been formed after the original episode of star formation – the gas was blown out of the cluster because of star light. Therefore, the brightest (shorterlived) stars have left the main sequence. Cluster age can be determined from the brightest stars still in th ...
... In globular clusters, no new stars have been formed after the original episode of star formation – the gas was blown out of the cluster because of star light. Therefore, the brightest (shorterlived) stars have left the main sequence. Cluster age can be determined from the brightest stars still in th ...
Discovery of extremely lead-rich subdwarfs: does heavy metal signal
... Hot subdwarfs represent a group of low-mass helium-burning stars formed through binarystar interactions and include some of the most chemically peculiar stars in the Galaxy. Stellar evolution theory suggests that they should have helium-rich atmospheres but, because radiation causes hydrogen to diff ...
... Hot subdwarfs represent a group of low-mass helium-burning stars formed through binarystar interactions and include some of the most chemically peculiar stars in the Galaxy. Stellar evolution theory suggests that they should have helium-rich atmospheres but, because radiation causes hydrogen to diff ...
Slide 1
... First epoch M31 is from some of the “deepest-ever” images: 100 ksec= 28 hours per filter. Those images were also dithered. You probably need a few orbits per first-epoch in nearby objects, more than one field per object, and dithering (though you can relax any of those constraints as desperation set ...
... First epoch M31 is from some of the “deepest-ever” images: 100 ksec= 28 hours per filter. Those images were also dithered. You probably need a few orbits per first-epoch in nearby objects, more than one field per object, and dithering (though you can relax any of those constraints as desperation set ...
Lecture Outline: Spectroscopy (Ch. 3.5 + 4)
... individual atoms, but now for large blobs of gas, like winds in the atmosphere. When you look at some gas in the atmosphere of a star or planet, these motions are much smaller than the region you can resolve, so the Doppler shifts from each of the randomly moving blobs are all blended together, like ...
... individual atoms, but now for large blobs of gas, like winds in the atmosphere. When you look at some gas in the atmosphere of a star or planet, these motions are much smaller than the region you can resolve, so the Doppler shifts from each of the randomly moving blobs are all blended together, like ...
*Studying Complex Star-Forming Fields: Rosette Nebula and Monoceros Loop by Chris Hathaway and Anthony Kuchera
... massive, recently born stars. About 5º north of Rosetta, the young open cluster NGC 2264 and the more compact Mon OB1 association seem to be spatially connected to the diffuse Cone Nebula (Herbst 1980). The positional coincidence of stars of the Mon OB2 association with the Monoceros Loop suggests t ...
... massive, recently born stars. About 5º north of Rosetta, the young open cluster NGC 2264 and the more compact Mon OB1 association seem to be spatially connected to the diffuse Cone Nebula (Herbst 1980). The positional coincidence of stars of the Mon OB2 association with the Monoceros Loop suggests t ...
VLT/FORS Surveys of Wolf-Rayet Stars beyond the
... (Chandar et al. 2004). This LMC-metallicity galaxy is dominated by a central starburst region which consists of two main emission knots, NGC 3125-A and -B, shown in Figure 4. From UV spectroscopy, Chandar et al. (2004) estimated 5 000 WR stars for a cluster within knot A, with a remarkable N(WR)/N(O ...
... (Chandar et al. 2004). This LMC-metallicity galaxy is dominated by a central starburst region which consists of two main emission knots, NGC 3125-A and -B, shown in Figure 4. From UV spectroscopy, Chandar et al. (2004) estimated 5 000 WR stars for a cluster within knot A, with a remarkable N(WR)/N(O ...
Stars and Their Characteristics
... Stars that show variation in brightness are known as variable stars. Distances in space are measured in astronomical units, light-years, and parsecs. Light-Year The distance that light travels in ...
... Stars that show variation in brightness are known as variable stars. Distances in space are measured in astronomical units, light-years, and parsecs. Light-Year The distance that light travels in ...
Lecture7
... eventually end up as white dwarfs. However, before the degeneracy sets in finally in the core, elements heavier than C and O would be synthesized. So, their core will consist of elements heavier than C and O, e.g., Mg, Si, but not Fe. However, some calculations show that some of these stars on the h ...
... eventually end up as white dwarfs. However, before the degeneracy sets in finally in the core, elements heavier than C and O would be synthesized. So, their core will consist of elements heavier than C and O, e.g., Mg, Si, but not Fe. However, some calculations show that some of these stars on the h ...
Surveying the Stars
... • What is a Hertzsprung–Russell diagram? — An H-R diagram plots the stellar luminosity of stars versus surface temperature (or color or spectral type). ...
... • What is a Hertzsprung–Russell diagram? — An H-R diagram plots the stellar luminosity of stars versus surface temperature (or color or spectral type). ...
EarthComm_c1s9
... have to get above Earth’s atmosphere. The Hubble Space Telescope, for example, can detect objects as dim as 30th magnitude. Perhaps you have seen a star described as a G-type star or an O-type star. This is a way of classifying stars that depends on the color and temperature of the star. They also h ...
... have to get above Earth’s atmosphere. The Hubble Space Telescope, for example, can detect objects as dim as 30th magnitude. Perhaps you have seen a star described as a G-type star or an O-type star. This is a way of classifying stars that depends on the color and temperature of the star. They also h ...
File
... * Nuclear Fusion in Massive Stars * At higher temperatures than carbon fusion, nuclei of oxygen, neon, and magnesium fuse to make silicon and sulfur. ...
... * Nuclear Fusion in Massive Stars * At higher temperatures than carbon fusion, nuclei of oxygen, neon, and magnesium fuse to make silicon and sulfur. ...
SMMP_BISANA - Infinity and Beyond
... The brightness of a star depends on both its size and its temperature. How bright a star looks from Earth depends on both its distance and how bright the star actually is. The brightness of a star can be described in 2 different ways: apparent brightness and absolute brightness. A star’s apparent br ...
... The brightness of a star depends on both its size and its temperature. How bright a star looks from Earth depends on both its distance and how bright the star actually is. The brightness of a star can be described in 2 different ways: apparent brightness and absolute brightness. A star’s apparent br ...
White dwarfs from GAIA: The 7th dimension
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
Introduction
... and at some moment becomes high enough to begin helium burning in the core (hydrogen burning continues in the shell), placing the star on the Horizontal Branch (HB). In stars with masses .2.5M helium burning is degenerate (helium-flashes). The helium burning results in a degenerate carbon and oxyge ...
... and at some moment becomes high enough to begin helium burning in the core (hydrogen burning continues in the shell), placing the star on the Horizontal Branch (HB). In stars with masses .2.5M helium burning is degenerate (helium-flashes). The helium burning results in a degenerate carbon and oxyge ...
Red Dwarf Stars: Ages, Rotation, Magnetic
... pre-main sequence stars and close binaries in the sample. Also in this study, we exclude spectral types later than ∼M7 because they appear to have Age-Rotation-Activity relations quite different to earlier spectral types. From a limited sample of M7–9 V stars, it appears that they do not undergo mag ...
... pre-main sequence stars and close binaries in the sample. Also in this study, we exclude spectral types later than ∼M7 because they appear to have Age-Rotation-Activity relations quite different to earlier spectral types. From a limited sample of M7–9 V stars, it appears that they do not undergo mag ...
Presentation - Relativity Group
... humans age by observing the humans living in a village at one time. • What two basic physical properties do astronomers use to classify stars? • Stars are classified by their luminosity and surface temperature. These properties, in turn, depend primarily on a star’s mass and its stage of life. ...
... humans age by observing the humans living in a village at one time. • What two basic physical properties do astronomers use to classify stars? • Stars are classified by their luminosity and surface temperature. These properties, in turn, depend primarily on a star’s mass and its stage of life. ...
AUGUSTE COMTE`S BLUNDER: AN ACCOUNT OF THE FIRST
... Abstract: In 1835 the French philosopher Auguste Comte predicted that we would never know anything about the chemical composition of stars. This paper gives a broad overview of the development of stellar spectroscopy, especially from about 1860. Developments in stellar spectroscopy segregated quite ...
... Abstract: In 1835 the French philosopher Auguste Comte predicted that we would never know anything about the chemical composition of stars. This paper gives a broad overview of the development of stellar spectroscopy, especially from about 1860. Developments in stellar spectroscopy segregated quite ...
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.