Determining the Sizes & Distances of Stars Using the H
... mass loss causes the star to eject its outer layers, which continue expanding out into space to form a planetary nebulae. For example, a star like the Sun will loose approximately 60% of its mass as it evolves to become a white dwarf. White dwarfs are low in luminosity, because fusion can no longer ...
... mass loss causes the star to eject its outer layers, which continue expanding out into space to form a planetary nebulae. For example, a star like the Sun will loose approximately 60% of its mass as it evolves to become a white dwarf. White dwarfs are low in luminosity, because fusion can no longer ...
File - We All Love Science
... – Hot, compact stars. Mass of about our Sun but radius of our Earth (about 1% of the Sun) – Little surface area means they are dim, even though hot – Light not from burning fuel, as none is left – Light from residual heat as they cool – Temps range from 25,000K-4,000K ...
... – Hot, compact stars. Mass of about our Sun but radius of our Earth (about 1% of the Sun) – Little surface area means they are dim, even though hot – Light not from burning fuel, as none is left – Light from residual heat as they cool – Temps range from 25,000K-4,000K ...
Still Lost in Space
... Could all these “stars” be basically the same type of object, only lying at different distances? Perhaps they are extremely compact emission-line nebulae. Normally any nebula would emit multiple lines, but perhaps these nebulae contain only one element, and very unusual excitation mechanisms, so ...
... Could all these “stars” be basically the same type of object, only lying at different distances? Perhaps they are extremely compact emission-line nebulae. Normally any nebula would emit multiple lines, but perhaps these nebulae contain only one element, and very unusual excitation mechanisms, so ...
Chapter 5 Notes
... b. Core contracts and heats up causing outer layers to _______ and cool c. Star becomes a _______ as it expands and outer layers cool ...
... b. Core contracts and heats up causing outer layers to _______ and cool c. Star becomes a _______ as it expands and outer layers cool ...
PHYSICS 1500 - ASTRONOMY TOTAL: 100 marks Section A Please
... Question 15 Why does the disk of our galaxy appear blue? (a) all the red starlight is scattered out of our view. (b) the blue light is recombination radiation from HII regions. (c) the blue light is emission from elements in the interstellar medium heavier than hydrogen. (d) it is illuminated by the ...
... Question 15 Why does the disk of our galaxy appear blue? (a) all the red starlight is scattered out of our view. (b) the blue light is recombination radiation from HII regions. (c) the blue light is emission from elements in the interstellar medium heavier than hydrogen. (d) it is illuminated by the ...
Introduction to Astronomy
... brightness. Antares has mag. 1; Polaris has mag. 2; naked eye limit is about 6. Sirius has mag. –1.5. • “Absolute magnitude” is a measure of true brightness. It’s what the apparent magnitude would be if the star were 33 light-years away. Sun’s absolute magnitude is about 5. • The formulas that relat ...
... brightness. Antares has mag. 1; Polaris has mag. 2; naked eye limit is about 6. Sirius has mag. –1.5. • “Absolute magnitude” is a measure of true brightness. It’s what the apparent magnitude would be if the star were 33 light-years away. Sun’s absolute magnitude is about 5. • The formulas that relat ...
Star - Uplift Education
... Suppose I observe with my telescope two red stars A and B that are part of a binary star system. Star A is 9 times brighter than star B. What can we say about their relative sizes and temperatures? Since both are red (the same color), the spectra peak at the same wavelength. ...
... Suppose I observe with my telescope two red stars A and B that are part of a binary star system. Star A is 9 times brighter than star B. What can we say about their relative sizes and temperatures? Since both are red (the same color), the spectra peak at the same wavelength. ...
Lecture 7 February 9
... 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 ...
Sample multiple choice questions for Exam 2
... PART I: Multiple Choice: 40 questions, 2 points each. Select the best answer to each of the questions below. Place your answer on the computer answer sheet provided. 1. Most of the bright stars in the sky are bright because they are close (within 10 light years) to our Sun. a) correct b) wrong: Most ...
... PART I: Multiple Choice: 40 questions, 2 points each. Select the best answer to each of the questions below. Place your answer on the computer answer sheet provided. 1. Most of the bright stars in the sky are bright because they are close (within 10 light years) to our Sun. a) correct b) wrong: Most ...
StarIntro_sb12
... The cooler red stars have longer wavelengths and may be only detected with infrared telescopes The hot blue stars have shorter wavelengths may be detected with ultraviolet or x-ray telescopes ...
... The cooler red stars have longer wavelengths and may be only detected with infrared telescopes The hot blue stars have shorter wavelengths may be detected with ultraviolet or x-ray telescopes ...
On the nature of early-type emission line objects in NGC6611
... close to the ZAMS. However, the analysis of our results demonstrates that a group (intermediate mass stars) of our NGC6611 targets have an age too old for the age of this star-formation region. Consequently, these stars must be, in fact, considered as pre-main sequence stars (PMS), which go to reach ...
... close to the ZAMS. However, the analysis of our results demonstrates that a group (intermediate mass stars) of our NGC6611 targets have an age too old for the age of this star-formation region. Consequently, these stars must be, in fact, considered as pre-main sequence stars (PMS), which go to reach ...
Stars: Their Life and Afterlife
... with masses of 104 – 106 MŸ. They are not necessarily gravitationally bound and, like all clouds in the galaxy, are transient structures with lifetimes on the scale of 10’s of millions of years. Their lifetimes are linked to the time scales of stellar formation, which seems natural since the formati ...
... with masses of 104 – 106 MŸ. They are not necessarily gravitationally bound and, like all clouds in the galaxy, are transient structures with lifetimes on the scale of 10’s of millions of years. Their lifetimes are linked to the time scales of stellar formation, which seems natural since the formati ...
AyC10 Fall 2007: Midterm 2 Review Sheet
... What does it mean for a star to be on the Main Sequence? A star is on the Main Sequence when its core is fusing hydrogen into helium. During this phase, stars are mostly stable and obey well-defined relationships between their mass, luminosity, and surface temperature (note: L M4 only applies to M ...
... What does it mean for a star to be on the Main Sequence? A star is on the Main Sequence when its core is fusing hydrogen into helium. During this phase, stars are mostly stable and obey well-defined relationships between their mass, luminosity, and surface temperature (note: L M4 only applies to M ...
Stages of stars - University of Dayton
... >May remain on main sequence for up to 100 billion years >Never evolve to become bloated red giants >Remain as stable main sequence stars until they consume their hydrogen fuel and collapse into white dwarfs Death of Massive Stars: >Have relatively short life spans >Terminate in an explosion known a ...
... >May remain on main sequence for up to 100 billion years >Never evolve to become bloated red giants >Remain as stable main sequence stars until they consume their hydrogen fuel and collapse into white dwarfs Death of Massive Stars: >Have relatively short life spans >Terminate in an explosion known a ...
Chapter11
... In this chapter, we use the laws of physics in a new way. We develop theories and models based on physics that help us understand how stars work. For instance, what stops a contracting star and gives it stability? We can understand this phenomenon because we understand some of the basic laws of phys ...
... In this chapter, we use the laws of physics in a new way. We develop theories and models based on physics that help us understand how stars work. For instance, what stops a contracting star and gives it stability? We can understand this phenomenon because we understand some of the basic laws of phys ...
STAR FORMATION (Ch. 19)
... pillars (emission nebulae), followed by circumstellar disks, and progressing to evolved massive stars in the young starburst cluster.To the upper right of center is the evolved blue supergiant called Sher 25. The star has a unique circumstellar ring of glowing gas that is a galactic twin to the famo ...
... pillars (emission nebulae), followed by circumstellar disks, and progressing to evolved massive stars in the young starburst cluster.To the upper right of center is the evolved blue supergiant called Sher 25. The star has a unique circumstellar ring of glowing gas that is a galactic twin to the famo ...
MS Word
... The stars in Table 2 are called Giants, and their spectral types are written with a III, such as K2III. Add a III to each of the spectral types in Table 2. The list of luminosity classes is given as follows: List of luminosity classes. Luminosity Class Ia and Ib II III IV V ...
... The stars in Table 2 are called Giants, and their spectral types are written with a III, such as K2III. Add a III to each of the spectral types in Table 2. The list of luminosity classes is given as follows: List of luminosity classes. Luminosity Class Ia and Ib II III IV V ...
Why are Binary Stars so Important for the Theory
... eclipsing binaries with the 50 cm reflecting telescope at La Silla belonging to the Copenhagen Observatory. Further there was the possibility of obtaining accurate spectroscopic elements from 12 A/mm plates using the ESO 1.5 m telescope. Extremely many observations of eclipsing binaries of all sorts ...
... eclipsing binaries with the 50 cm reflecting telescope at La Silla belonging to the Copenhagen Observatory. Further there was the possibility of obtaining accurate spectroscopic elements from 12 A/mm plates using the ESO 1.5 m telescope. Extremely many observations of eclipsing binaries of all sorts ...
earth & space science
... Classifying Stars Main sequence is the location on the H-R diagram where most stars lie; it has a diagonal pattern from the lower right to the upper left. One way scientists classify stars is by plotting the surface temperatures of stars against their ...
... Classifying Stars Main sequence is the location on the H-R diagram where most stars lie; it has a diagonal pattern from the lower right to the upper left. One way scientists classify stars is by plotting the surface temperatures of stars against their ...
LESSON 4, STARS
... The Sun is far less than a light year away. The reason is that a light year is the distance that light travels in a year. Light from the Sun takes 8 minutes to reach Earth, which is much less than a year. ...
... The Sun is far less than a light year away. The reason is that a light year is the distance that light travels in a year. Light from the Sun takes 8 minutes to reach Earth, which is much less than a year. ...
mass of star
... The proton and electron each have “spin”. A result from quantum mechanics: if both spinning the same way, atom's energy is slightly higher. Eventually will make transition to state of opposite spins. Energy difference is small -> radio photon emitted, wavelength 21-cm. ...
... The proton and electron each have “spin”. A result from quantum mechanics: if both spinning the same way, atom's energy is slightly higher. Eventually will make transition to state of opposite spins. Energy difference is small -> radio photon emitted, wavelength 21-cm. ...
Mr. Traeger`s Light and Stars PowerPoint
... scientists can determine what elements are present in the cooler gas that is absorbing some of the light.” ...
... scientists can determine what elements are present in the cooler gas that is absorbing some of the light.” ...
Document
... the same time. • The cluster is as old as the most luminous (massive) star left on the MS. • All MS stars to the left have already used up their H fuel and are gone. • The position of the hottest, brightest star on a cluster’s main sequence is called the main sequence turnoff point. ...
... the same time. • The cluster is as old as the most luminous (massive) star left on the MS. • All MS stars to the left have already used up their H fuel and are gone. • The position of the hottest, brightest star on a cluster’s main sequence is called the main sequence turnoff point. ...
Astro 10 Practice Test 2
... 34. Notice that along the top edge of this graph, the letter names of the spectral classes have been blurred out. What is the correct order of the spectral classes, from left to right? a. MGAKFOB b. OBAGKMF c. ABCFGKM d. OBAFGKM ...
... 34. Notice that along the top edge of this graph, the letter names of the spectral classes have been blurred out. What is the correct order of the spectral classes, from left to right? a. MGAKFOB b. OBAGKMF c. ABCFGKM d. OBAFGKM ...
Blackbody Radiation, Stellar temperature and types
... Stars are classified according to their surface or color temperature. Spectral types are OBAFGMK with a digit 0 to 9 in order from hottest (O1) to coolest (K9). A Roman numeral is added to the classification to indicate size: I = giant to V = dwarf. ...
... Stars are classified according to their surface or color temperature. Spectral types are OBAFGMK with a digit 0 to 9 in order from hottest (O1) to coolest (K9). A Roman numeral is added to the classification to indicate size: I = giant to V = dwarf. ...
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.