Main Sequence stars
... Together Saha and PayneGaposchkin • Gave theoretical explanation for Cannon’s classification scheme. • Showed that the differences in spectra (absorption lines) are due to temperature and thermal ionization of atoms not abundance of elements • Provided a convincing argument that stars are mostly ma ...
... Together Saha and PayneGaposchkin • Gave theoretical explanation for Cannon’s classification scheme. • Showed that the differences in spectra (absorption lines) are due to temperature and thermal ionization of atoms not abundance of elements • Provided a convincing argument that stars are mostly ma ...
What is a Scientist? - Cockeysville Middle School
... Which characteristics do you think will be easiest to learn about? Why? Astronomers classify stars according to physical characteristics. Skim text page 127 to identify 5 characteristics that astronomers use to classify stars. ...
... Which characteristics do you think will be easiest to learn about? Why? Astronomers classify stars according to physical characteristics. Skim text page 127 to identify 5 characteristics that astronomers use to classify stars. ...
lecture12
... A classification of the stellar black body For historical reasons, astronomers classify the temperatures of stars on a scale defined by spectral types, called O B A F G K M, ranging from the hottest (type O) to the coolest (type M) stars. ...
... A classification of the stellar black body For historical reasons, astronomers classify the temperatures of stars on a scale defined by spectral types, called O B A F G K M, ranging from the hottest (type O) to the coolest (type M) stars. ...
A Star is “Born,” and then How Will it Move
... Young (Embedded) Clusters: Very young (<10 Myr-old) groups of young stars that form together. Future binding depends on cluster mass & velocity, seems that 90% dissolve before ~10 Myr (Lada & Lada 2003). When they unbind but are still seen to move together, they’re known as a “stellar association.” ...
... Young (Embedded) Clusters: Very young (<10 Myr-old) groups of young stars that form together. Future binding depends on cluster mass & velocity, seems that 90% dissolve before ~10 Myr (Lada & Lada 2003). When they unbind but are still seen to move together, they’re known as a “stellar association.” ...
Chapter16
... spectral lines. solar motion — The motion of the Sun with respect to the nearby stars. spectral class — A categorization, based on the pattern of spectral lines of stars, that groups stars according to their surface temperatures. supergiant — An extremely luminous star of large size and mass. white ...
... spectral lines. solar motion — The motion of the Sun with respect to the nearby stars. spectral class — A categorization, based on the pattern of spectral lines of stars, that groups stars according to their surface temperatures. supergiant — An extremely luminous star of large size and mass. white ...
The Life of Stars
... blood, and the carbon in our apple pies were all made in the interior of collapsing stars. We are made of ...
... blood, and the carbon in our apple pies were all made in the interior of collapsing stars. We are made of ...
Powerpoint of lecture 1
... 6 magnitude classes (1 brightest, 6 just visible) Norman Pogson (~1850): defined apparent magnitude m by m = constant – 2.5 log10F , choosing constant to make scale consistent with Hipparchus. Absolute magnitude M is defined as the apparent magnitude a star ...
... 6 magnitude classes (1 brightest, 6 just visible) Norman Pogson (~1850): defined apparent magnitude m by m = constant – 2.5 log10F , choosing constant to make scale consistent with Hipparchus. Absolute magnitude M is defined as the apparent magnitude a star ...
Stars
... The Blue Supergiants will begin to burn up all of the hydrogen that they have after a few million years. When this happens, the outer shell of the star begins to expand. It grows to about triple the size that it currently is. The Blue Supergiant now becomes a Supergiant. Supergiants are orange/yello ...
... The Blue Supergiants will begin to burn up all of the hydrogen that they have after a few million years. When this happens, the outer shell of the star begins to expand. It grows to about triple the size that it currently is. The Blue Supergiant now becomes a Supergiant. Supergiants are orange/yello ...
The Death of Stars
... • Most of the iron in our Universe is from Type Ia supernova. • Because all the Type Ia supernovae ignite at a similar mass (1.4Msun), they have similar luminosities: they are standard candles! • They are really bright 5 billion times brighter than our Sun: so we see them at huge distances. • By com ...
... • Most of the iron in our Universe is from Type Ia supernova. • Because all the Type Ia supernovae ignite at a similar mass (1.4Msun), they have similar luminosities: they are standard candles! • They are really bright 5 billion times brighter than our Sun: so we see them at huge distances. • By com ...
HR Diagram Activity - Mr. Alster`s Science Classes
... 10. Overall, are the stars in Group 3 very bright or very dim? 11. Are these stars hot or cool compared to other stars? 12. Is the relationship of brightness to temperature for these stars puzzling, or does it make sense? Explain. Additional Questions 13. As you can see from the Group 1 stars, the ...
... 10. Overall, are the stars in Group 3 very bright or very dim? 11. Are these stars hot or cool compared to other stars? 12. Is the relationship of brightness to temperature for these stars puzzling, or does it make sense? Explain. Additional Questions 13. As you can see from the Group 1 stars, the ...
STUDY GUIDE FOR CHAPTER 1
... A. They go through first red giant, helium burning in the core, and double shell burning phases. B. Then they go through a sequence of situations where the core is contracting and heating up when no fusion is going on inside it and then stops contracting when the next type of fusion begins. Meanwhil ...
... A. They go through first red giant, helium burning in the core, and double shell burning phases. B. Then they go through a sequence of situations where the core is contracting and heating up when no fusion is going on inside it and then stops contracting when the next type of fusion begins. Meanwhil ...
HR Diagram Lab
... 1. What would you tell someone who thinks that all stars are very similar (be sure to discuss temperature and brightness)? 2. How does our sun compare to other stars in brightness and temperature? 3. Are the stars scattered randomly on the graph, or is there a pattern? Explain. 4. Would you expect h ...
... 1. What would you tell someone who thinks that all stars are very similar (be sure to discuss temperature and brightness)? 2. How does our sun compare to other stars in brightness and temperature? 3. Are the stars scattered randomly on the graph, or is there a pattern? Explain. 4. Would you expect h ...
Distances to Stars: Parsecs and Light Years
... How far away are they? How hot are they? How massive are they What are they made of? Do they have planets too? How do they change with time (stellar evolution) ...
... How far away are they? How hot are they? How massive are they What are they made of? Do they have planets too? How do they change with time (stellar evolution) ...
Star Formation/Llfe Cycle Notes
... bouncing off each other, increasing pressure, and temp and slowing contraction) c. Known as Protostar of YSO, before it reaches main sequence d. Center of protostar gets dense enough and therefore hot enough (3000K+) to become luminous, however not visible due to exterior of gas and dust surrounding ...
... bouncing off each other, increasing pressure, and temp and slowing contraction) c. Known as Protostar of YSO, before it reaches main sequence d. Center of protostar gets dense enough and therefore hot enough (3000K+) to become luminous, however not visible due to exterior of gas and dust surrounding ...
Document
... larger Because giant and supergiant stars have such huge surface areas to give off light, they are very bright ...
... larger Because giant and supergiant stars have such huge surface areas to give off light, they are very bright ...
Our Sun - STEMpire Central
... D) OBAFGKM 6. More massive stars can be found where on the HR Diagram? A) The top B) The bottom C) The center D) In the corners Draw an HR Diagram. Include the following: 1. The four measured aspects along each side, showing the direction of increasing value. 2. The regions on the diagram where one ...
... D) OBAFGKM 6. More massive stars can be found where on the HR Diagram? A) The top B) The bottom C) The center D) In the corners Draw an HR Diagram. Include the following: 1. The four measured aspects along each side, showing the direction of increasing value. 2. The regions on the diagram where one ...
ASTR-1020: Astronomy II Course Lecture Notes - Faculty
... (A0 V) will remain for 370 million years (Vega is relatively young), and an M0 V star will remain on the main sequence for 57 billion years! Since the Universe is about 12-14 billion years old, no M0 star has yet evolved off of the main sequence. ...
... (A0 V) will remain for 370 million years (Vega is relatively young), and an M0 V star will remain on the main sequence for 57 billion years! Since the Universe is about 12-14 billion years old, no M0 star has yet evolved off of the main sequence. ...
Chapter 30 Section 2 Handout
... What does increased temperature from contraction in the core cause the helium core to do? ...
... What does increased temperature from contraction in the core cause the helium core to do? ...
10.1 The Solar Neighborhood Barnard`s Star
... The darkened curve is called the Main Sequence, as this is where most stars are. Also indicated is the white dwarf region; these stars are hot but not very luminous, as they are quite small. ...
... The darkened curve is called the Main Sequence, as this is where most stars are. Also indicated is the white dwarf region; these stars are hot but not very luminous, as they are quite small. ...
3.1 Introduction
... 0 to 9. Thus we have spectral classes O9 and B0, the former being just hotter than the latter. Division between subclasses can be finer, e.g. class O9.5. O and B stars are sometimes referred to as ‘early-type’, while K and M are ‘late-type’. The Sun has spectral class G2. More recently the classific ...
... 0 to 9. Thus we have spectral classes O9 and B0, the former being just hotter than the latter. Division between subclasses can be finer, e.g. class O9.5. O and B stars are sometimes referred to as ‘early-type’, while K and M are ‘late-type’. The Sun has spectral class G2. More recently the classific ...
Stars Unit 1-2: Stars
... • Luminosity depends on the stars temperature and size. • Apparent magnitude depends on the distance from the star to the Earth. • Example: – A 100W light bulb has a higher luminosity than a 20W flashlight bulb. – But if that flashlight bulb is right in front of your eye, it will appear brighter tha ...
... • Luminosity depends on the stars temperature and size. • Apparent magnitude depends on the distance from the star to the Earth. • Example: – A 100W light bulb has a higher luminosity than a 20W flashlight bulb. – But if that flashlight bulb is right in front of your eye, it will appear brighter tha ...
chapter6
... Just by analyzing the light received from a star, astronomers can retrieve information about a star’s ...
... Just by analyzing the light received from a star, astronomers can retrieve information about a star’s ...
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.