Transcript Take time to understand it now

Astronomy 1020-H
Stellar Astronomy
Spring_2016
Day-14
Solar Flare
Course Announcements
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1st “Hot Topics in Science”: Coming soon …
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Topics this semester are: Human Cloning, Environmental
Toxicology, & Fracking … includes pizza.
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Dark Night Observing: Mon. 2/29 & Wed. 3/2 –
7:30pm at the APSU Observatory
Exam-2 – Fri. 3/4 Chapters 5 & 6
Smartworks Chapters 5 & 6: Due Fri. 3/4
Spring Break Mar. 5-13 (Sat.-Sun.)
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APSU Research and Creativity Forum April 15, 2016
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Abstracts are due: 4:00pm Fri., March 18
Feb. 29 – Last day to drop with an automatic “W”
Apr. 1 – Last day to drop a class with W, F, FA
Course Announcements
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Colloquium TODAY, Feb. 19. @3:00pm B310
Dr. David James, Cerro-Tololo InterAmerican Obs.
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Open Clusters, Stellar Evolution and Calibrating the Ages
of Stars: Blanco 1
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Galactic open clusters are laboratories, provided by nature, for
us to study stellar evolution. Using 1m-, 4m- and 8m-class
telescopes, I will show how spectroscopic and photometric
observations of solar-type stars in open clusters allow us to
establish a stellar chronometer, and create an age-ranking
system for an ensemble of nearby, well-studied clusters. With
the aid of new observations of Blanco 1, an high-Galactic
latitude, Pleiades-age cluster, I will show how deriving stellar
age must be based upon very high quality observational data
and a diverse range of stellar models.
 The spectrum of
a cloud of
glowing gas
contains
emission lines.
 When viewed
through a cloud
of gas, a
continuous
spectrum will
have absorption
lines.
Lecture Tutorial
Types of Spectra: (pg. 63)
• Work with a partner!
• Read the instructions and questions carefully.
• Discuss the concepts and your answers with one
another. Take time to understand it now!!!!
• Come to a consensus answer you both agree on.
• If you get stuck or are not sure of your answer, ask
another group.
 The wavelengths at which atoms emit and
absorb radiation form unique spectral
fingerprints for each atom.
 They help determine a star’s composition,
temperature, and more.
 The motion of a light source toward or away
from us changes our perception of the
wavelength of the waves reaching us.
 Doppler effect.
MATH TOOLS 5.2
 If you know the wavelength of light you are
observing as well as the wavelength of light
the object would be emitting if it were at rest,
you can find the speed of the object using
the Doppler effect.
 Light from approaching objects is
blueshifted; the waves crowd together.
 Light from receding objects is redshifted;
the waves are spaced farther apart.
 The motion of a light source toward or away
from us changes our perception of the
wavelength of the waves reaching us.
 Doppler effect.
Lecture Tutorial
Doppler Shift: (pg. 75)
• Work with a partner!
• Read the instructions and questions carefully.
• Discuss the concepts and your answers with one
another. Take time to understand it now!!!!
• Come to a consensus answer you both agree on.
• If you get stuck or are not sure of your answer, ask
another group.