Stars, Galaxies, and the Universe
... Consists mostly of hydrogen and it turns into helium to produce energy This change is created when hydrogen particles collide (fusion) The energy is the source of light and warmth that make life possible on Earth ...
... Consists mostly of hydrogen and it turns into helium to produce energy This change is created when hydrogen particles collide (fusion) The energy is the source of light and warmth that make life possible on Earth ...
Forging the elements
... Russell Diagram The HR diagram was first plotted by Hertzsprung (1911) and Russell (1913). It is used to study the evolution and properties of stars. The HR diagram is a plot of : Stellar Luminosity or Absolute Magnitude (y-axis) ...
... Russell Diagram The HR diagram was first plotted by Hertzsprung (1911) and Russell (1913). It is used to study the evolution and properties of stars. The HR diagram is a plot of : Stellar Luminosity or Absolute Magnitude (y-axis) ...
Lecture 10: The Hertzsprung
... See also Figure 19-21 in your book There is a mass-luminosity relation on the main sequence. We can use that + a sample of stars where we get all the stars within a certain distance of the Sun to figure out how many stars of what masses are out there. Answer: Lots of low-mass stars! Very few high-m ...
... See also Figure 19-21 in your book There is a mass-luminosity relation on the main sequence. We can use that + a sample of stars where we get all the stars within a certain distance of the Sun to figure out how many stars of what masses are out there. Answer: Lots of low-mass stars! Very few high-m ...
Review for Midterm 1
... 5. Lives of stars: What do stars do while in the “main sequence”? How and why do mass affect the expected lifetime of a star? What is the difference between the size of a star and the size of our galaxy? 6. Deaths of Stars: What is the fate of the sun in about 6 billion years? What will save the sun ...
... 5. Lives of stars: What do stars do while in the “main sequence”? How and why do mass affect the expected lifetime of a star? What is the difference between the size of a star and the size of our galaxy? 6. Deaths of Stars: What is the fate of the sun in about 6 billion years? What will save the sun ...
General Introduction 1. Luminosity, Flux and Magnitude The
... of the inclination angle. The size of the orbit can thus be inferred. Individual masses can be determined in cases where two sets of spectral lines appear and the inclination angle can also be established. The quantity M = 1.989 × 1033 g is the solar mass. A correlation (MS) exists between the stel ...
... of the inclination angle. The size of the orbit can thus be inferred. Individual masses can be determined in cases where two sets of spectral lines appear and the inclination angle can also be established. The quantity M = 1.989 × 1033 g is the solar mass. A correlation (MS) exists between the stel ...
Stars
... outward forces must balance. If they don't, the shell will either collapse or expand. The mystery timescale for this to occur is called the "free-fall timescale," and it is about 2,000 seconds for a star like the Sun. Since we know the Sun has been essentially stable over Star Life the age of Earth ...
... outward forces must balance. If they don't, the shell will either collapse or expand. The mystery timescale for this to occur is called the "free-fall timescale," and it is about 2,000 seconds for a star like the Sun. Since we know the Sun has been essentially stable over Star Life the age of Earth ...
AST 301 Introduction to Astronomy - University of Texas Astronomy
... Temperature-Luminosity diagrams Astronomers measure the temperatures and luminosities of many stars and plot them on a diagram called the Hertzsprung-Russell (or H-R) diagram. For historical reasons they plot temperatures increasing to the left (not right) and luminosities increasing upward. They a ...
... Temperature-Luminosity diagrams Astronomers measure the temperatures and luminosities of many stars and plot them on a diagram called the Hertzsprung-Russell (or H-R) diagram. For historical reasons they plot temperatures increasing to the left (not right) and luminosities increasing upward. They a ...
GEARS Workshop Monday - Georgia Southern University
... High mass stars fusion Hydrogen to Helium So do low mass stars Stars are made up primarily of Hydrogen So… high mass stars should have lots more hydrogen to fuse than low mass stars • How come high mass stars fuse hydrogen for so much less time? ...
... High mass stars fusion Hydrogen to Helium So do low mass stars Stars are made up primarily of Hydrogen So… high mass stars should have lots more hydrogen to fuse than low mass stars • How come high mass stars fuse hydrogen for so much less time? ...
Introduction to the HR Diagram
... main sequence is also a function of its mass and luminosity and is defined as: T(years) = 1010M. L The Giant Branch: Red giants are luminous, cool giant stars in spectral classes F, G, K, and M located in the upper right-hand corner of the H-R diagram. As the central core of a main sequence star wit ...
... main sequence is also a function of its mass and luminosity and is defined as: T(years) = 1010M. L The Giant Branch: Red giants are luminous, cool giant stars in spectral classes F, G, K, and M located in the upper right-hand corner of the H-R diagram. As the central core of a main sequence star wit ...
Section 25.2 Stellar Evolution
... Match each death description with its star. Death Description 7. forms a red giant, which then collapses into a red dwarf and forms a planetary nebula 8. blows up in a supernova explosion 9. does not form a red giant; collapses directly into a white dwarf ...
... Match each death description with its star. Death Description 7. forms a red giant, which then collapses into a red dwarf and forms a planetary nebula 8. blows up in a supernova explosion 9. does not form a red giant; collapses directly into a white dwarf ...
Document
... and low-mass main sequence (hydrogen burning) stars like the Sun. • Protostars forms from molecular clouds. When a portion of a molecular cloud reaches a critical mass it begins to collapse under its own gravity. The initial collapse takes about 100,000 years. After that time the star reaches a surf ...
... and low-mass main sequence (hydrogen burning) stars like the Sun. • Protostars forms from molecular clouds. When a portion of a molecular cloud reaches a critical mass it begins to collapse under its own gravity. The initial collapse takes about 100,000 years. After that time the star reaches a surf ...
Pre-Main Sequence Evolution
... the disk has the lowest density (out the poles). These patches of nebulosity are called Herbig-Haro objects. ...
... the disk has the lowest density (out the poles). These patches of nebulosity are called Herbig-Haro objects. ...
Nebulae
... in the upper right region on an H-R diagram • Further evolution of a protostar causes it to move toward the main sequence on the H-R diagram • When its core temperatures become high enough to ignite steady hydrogen burning, it becomes a main sequence star ...
... in the upper right region on an H-R diagram • Further evolution of a protostar causes it to move toward the main sequence on the H-R diagram • When its core temperatures become high enough to ignite steady hydrogen burning, it becomes a main sequence star ...
Stars & Galaxies
... relatively small volume. A nebula, on the other hand, is a large amount of gas and dust spread out in an immense volume. ...
... relatively small volume. A nebula, on the other hand, is a large amount of gas and dust spread out in an immense volume. ...
Study Guide for 3RD Astronomy Exam
... List or identify the luminosity, mass, radius, temperature, and lifetime of an O main sequence star, the Sun and an M main sequence star. State the impact of convection in the envelope of very low mass stars on the stars main sequence lifetime. Describe or identify changes in a star during its main ...
... List or identify the luminosity, mass, radius, temperature, and lifetime of an O main sequence star, the Sun and an M main sequence star. State the impact of convection in the envelope of very low mass stars on the stars main sequence lifetime. Describe or identify changes in a star during its main ...
Life on the Main Sequence + Expansion to Red Giant
... fly-ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). ...
... fly-ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). ...
stars
... which is well understood to originate from a flattened circumstellar disk (e.g. Struve, 1931), can come and go episodically on time scales of days to decades. ...
... which is well understood to originate from a flattened circumstellar disk (e.g. Struve, 1931), can come and go episodically on time scales of days to decades. ...
Lecture1
... The “parallax” is the apparent shift in position of a nearby star, relative to background stars, as Earth moves around the Sun in it’s orbit ...
... The “parallax” is the apparent shift in position of a nearby star, relative to background stars, as Earth moves around the Sun in it’s orbit ...
A-105 Homework 1
... 2. (1 pt.) How can the contraction of an inert helium core trigger the ignition of a hydrogen-fusion shell? ...
... 2. (1 pt.) How can the contraction of an inert helium core trigger the ignition of a hydrogen-fusion shell? ...
Universe 8e Lecture Chapter 17 Nature of Stars
... 17-7 How H-R diagrams summarize our knowledge of the stars 17-6 How stars come in a wide variety of sizes 17-8 How we can deduce a star’s size from its spectrum ...
... 17-7 How H-R diagrams summarize our knowledge of the stars 17-6 How stars come in a wide variety of sizes 17-8 How we can deduce a star’s size from its spectrum ...
Properties of Stars
... 2. Stars, although not perfect black bodies, are close enough so that Planck curves are useful descriptions of their radiation. ...
... 2. Stars, although not perfect black bodies, are close enough so that Planck curves are useful descriptions of their radiation. ...
L5 - QUB Astrophysics Research Centre
... The surface luminosity of the sun is L =3.86x1026W, and at no point in the Sun can the luminosity exceed this value (see eqn of energy production). What can you conclude from this ? As the T and v of the rising elements are determined by the difference between the actual temperature gradient and a ...
... The surface luminosity of the sun is L =3.86x1026W, and at no point in the Sun can the luminosity exceed this value (see eqn of energy production). What can you conclude from this ? As the T and v of the rising elements are determined by the difference between the actual temperature gradient and a ...
Lecture15
... • Red giants lose most of their envelopes in an expanding shell of low density gas (planetary nebula , ~10,000 years) ...
... • Red giants lose most of their envelopes in an expanding shell of low density gas (planetary nebula , ~10,000 years) ...