THE LIFE CYCLES OF STARS (3)
... Illust Objective Prism Spectra Each little spectrum on the plate needs microscopic examination Pickering found that ladies were much better at this job than men (and cheaper) and had an army known as the Harvard Ladies. They tried to classify the spectra into types. Illust Harvard Ladies They starte ...
... Illust Objective Prism Spectra Each little spectrum on the plate needs microscopic examination Pickering found that ladies were much better at this job than men (and cheaper) and had an army known as the Harvard Ladies. They tried to classify the spectra into types. Illust Harvard Ladies They starte ...
Homework #7 (Ch. 19)
... protostars are typically so cool that they generate primarily infrared light. 8. Chaisson Review and Discussion 19.14 What is a shock wave? Of what significance are shock waves in star formation? (3 points) Many processes, such as supernova explosions, spiral density waves, and radiation from hot st ...
... protostars are typically so cool that they generate primarily infrared light. 8. Chaisson Review and Discussion 19.14 What is a shock wave? Of what significance are shock waves in star formation? (3 points) Many processes, such as supernova explosions, spiral density waves, and radiation from hot st ...
DTU 8e Chap 11 Characterizing Stars
... ionized Helium (He II) lines. Several of the broad, dark bands in the spectrum of the coolest stars (M-type stars) are caused by titanium oxide (TiO) molecules, which can exist only if the temperature is below about 3700 K. ...
... ionized Helium (He II) lines. Several of the broad, dark bands in the spectrum of the coolest stars (M-type stars) are caused by titanium oxide (TiO) molecules, which can exist only if the temperature is below about 3700 K. ...
THE PROPERTIES OF MAIN-SEQUENCE STARS - Cosmos
... V and actually lie within 100 pc. From this subsample we can determine the distribution in MV of mainsequence stars of given spectral type for spectral types that range from early F to early K. These distributions are signi cantly non-Gaussian, but when tted to Gaussians they yield central values o ...
... V and actually lie within 100 pc. From this subsample we can determine the distribution in MV of mainsequence stars of given spectral type for spectral types that range from early F to early K. These distributions are signi cantly non-Gaussian, but when tted to Gaussians they yield central values o ...
Astronomy Study Guide
... Composition—73% hydrogen, 25% helium, 2% other Brightness— apparent brightness—very bright absolute brightness—average brightness ...
... Composition—73% hydrogen, 25% helium, 2% other Brightness— apparent brightness—very bright absolute brightness—average brightness ...
What is it? - Carmenes - Calar Alto Observatory
... Our Solar System has eight planets. Four of them are “terrestrial” planets: Mercury (with its Moon-like surface), Venus (with its greenhouse atmosphere), the Earth (with its living creatures) and Mars (with its volcanoes and canyons), while the other four are “gas giant” planets: Jupiter (with its R ...
... Our Solar System has eight planets. Four of them are “terrestrial” planets: Mercury (with its Moon-like surface), Venus (with its greenhouse atmosphere), the Earth (with its living creatures) and Mars (with its volcanoes and canyons), while the other four are “gas giant” planets: Jupiter (with its R ...
Apparent Magnitude
... Gliese catalog of nearby stars. An examination of the diagram shows that stars tend to fall only into certain regions on the diagram. The most predominant is the diagonal, going from the upper-left (hot and bright) to the lower-right (cooler and less bright), called the main sequence. In the lower-l ...
... Gliese catalog of nearby stars. An examination of the diagram shows that stars tend to fall only into certain regions on the diagram. The most predominant is the diagonal, going from the upper-left (hot and bright) to the lower-right (cooler and less bright), called the main sequence. In the lower-l ...
Stellar Populations of Galaxies- 2 Lectures H
... Classical indicators of what is going on: The limit of the Balmer series and the blending of the high-order Balmer lines produces a discontinuity of the spectrum blueward of 3650°A. (the Balmer break) –more important in young populations, The break amplitude and position is a proxy for the age of th ...
... Classical indicators of what is going on: The limit of the Balmer series and the blending of the high-order Balmer lines produces a discontinuity of the spectrum blueward of 3650°A. (the Balmer break) –more important in young populations, The break amplitude and position is a proxy for the age of th ...
Volcanoes and Igneous Activity Earth - Chapter 4
... magnitudes – dim stars have large numbers and negative numbers are also used ...
... magnitudes – dim stars have large numbers and negative numbers are also used ...
AS2001 - University of St Andrews
... • Lab measurements: Unique line signature for each element. ...
... • Lab measurements: Unique line signature for each element. ...
Time From the Perspective of a Particle Physicist
... like sugars, alcohol and amino acids) usually cold (100O K or -300O F) usually almost perfect vacuum with 1 atom/cm3 (1 g water = 1023 atoms) Local concentrations: compressed by gravity and form stars. Called Giant Molecular Clouds as molecules have been observed. Need about 1,000,000 times the mass ...
... like sugars, alcohol and amino acids) usually cold (100O K or -300O F) usually almost perfect vacuum with 1 atom/cm3 (1 g water = 1023 atoms) Local concentrations: compressed by gravity and form stars. Called Giant Molecular Clouds as molecules have been observed. Need about 1,000,000 times the mass ...
script
... The strength of the Lithium line can be calibrated with age, but it is generally not that good. In a solar type star the presence of Lithium most likely means it is young. But the processes that affect the strength of lithium are poorly known. For instance, strong Li is also found in some evolved gi ...
... The strength of the Lithium line can be calibrated with age, but it is generally not that good. In a solar type star the presence of Lithium most likely means it is young. But the processes that affect the strength of lithium are poorly known. For instance, strong Li is also found in some evolved gi ...
2. Stellar Physics
... • Radiates energy that is primarily released by nuclear fusion reactions in the stellar interior Other energy sources are dominant during star formation and stellar death: • Star formation - before the interior is hot enough for significant fusion, gravitational potential energy is radiated as the r ...
... • Radiates energy that is primarily released by nuclear fusion reactions in the stellar interior Other energy sources are dominant during star formation and stellar death: • Star formation - before the interior is hot enough for significant fusion, gravitational potential energy is radiated as the r ...
Lecture 22 - Seattle Central
... “The Initial Mass Function”: For every O star, there are ~200 K and M stars ...
... “The Initial Mass Function”: For every O star, there are ~200 K and M stars ...
Chapter 13 (Properties of Stars)
... C. Wavelength/temperature increasing to the right. D. Wavelength/temperature decreasing to the right. 15. Refer to the H-R diagram: for stars in general, a higher mass star may be found: A. at higher luminosity and lower temperature. B. at higher luminosity and higher temperature. C. observed at sho ...
... C. Wavelength/temperature increasing to the right. D. Wavelength/temperature decreasing to the right. 15. Refer to the H-R diagram: for stars in general, a higher mass star may be found: A. at higher luminosity and lower temperature. B. at higher luminosity and higher temperature. C. observed at sho ...
Volcanoes and Igneous Activity Earth
... 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. ...
Interstellar medium, birth and life of stars
... The most massive pre–main-sequence stars take the shortest time to become main-sequence stars (O and B stars). In the final stages of pre–main-sequence contraction, when hydrogen fusion is about to begin in the core, the pre–main-sequence star may undergo vigorous chromospheric activity that eje ...
... The most massive pre–main-sequence stars take the shortest time to become main-sequence stars (O and B stars). In the final stages of pre–main-sequence contraction, when hydrogen fusion is about to begin in the core, the pre–main-sequence star may undergo vigorous chromospheric activity that eje ...
The Physical Properties of Normal A Stars
... Si/log Sr, v sin i, and . My “model” was that stars rotating sufficiently fast have normal abundances all over their surfaces. When the rotation decreases below some critical value, the poles begin to show peculiar abundances. These regions with peculiar abundances increase with decreasing rotation ...
... Si/log Sr, v sin i, and . My “model” was that stars rotating sufficiently fast have normal abundances all over their surfaces. When the rotation decreases below some critical value, the poles begin to show peculiar abundances. These regions with peculiar abundances increase with decreasing rotation ...
Part 3
... the light curve is not equal causes： 1 Asymmetry of the common envelope 2 Stellar dark spots model 3 Hot spots model problems： 1 We don’t know which mechanism is dominant 2 We don’t know the reason(s) which caused the O’connell effect type changes ...
... the light curve is not equal causes： 1 Asymmetry of the common envelope 2 Stellar dark spots model 3 Hot spots model problems： 1 We don’t know which mechanism is dominant 2 We don’t know the reason(s) which caused the O’connell effect type changes ...
Stellar Evolution
... - a very large and bright star whose hot core has used most of its hydrogen. ...
... - a very large and bright star whose hot core has used most of its hydrogen. ...
the life cycles of stars (5) - U3A Bendigo Courses / Activities
... billion for the sun. These are O and B type stars. Even before leaving the main sequence these stars emit material from their surface due to sheer radiation pressure. The strong light radiation carries gas with it. Our sun emits a solar wind of protons and electrons which can cause aurorae and in ce ...
... billion for the sun. These are O and B type stars. Even before leaving the main sequence these stars emit material from their surface due to sheer radiation pressure. The strong light radiation carries gas with it. Our sun emits a solar wind of protons and electrons which can cause aurorae and in ce ...
Synthetic color-magnitude diagrams: the ingredients
... Up to now, there are few observational constraints on the overall mass-ratio distribution of the binary population. One of the few measures of f(q) for binary systems, comes from Fisher et al. (2005) who estimated the q distribution function from spectroscopic observations of field binaries within ...
... Up to now, there are few observational constraints on the overall mass-ratio distribution of the binary population. One of the few measures of f(q) for binary systems, comes from Fisher et al. (2005) who estimated the q distribution function from spectroscopic observations of field binaries within ...
Planetarium Activity 1 Learning to measure brightness and Limiting
... and Orion) fix their position in the sky when the lights are off so that its approximated location can be found as the lights brighten. Use dots to Sketch the constellations on your worksheet and connect the stars with dash line. 2. As the lights are raised the first time, note the relative order in ...
... and Orion) fix their position in the sky when the lights are off so that its approximated location can be found as the lights brighten. Use dots to Sketch the constellations on your worksheet and connect the stars with dash line. 2. As the lights are raised the first time, note the relative order in ...
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.