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Star brightness and star distance: Difference between revisions

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|topic=Astronomy
|topic=Astronomy
|subject=Science
|subject=Science
|tagline=A slide presentation to explain how we measure the distance and brightness of stars.
|tagline=A slide presentation to explain how we measure the distance
and brightness of stars.
|image=Starsandbrightness0.png
|image=Starsandbrightness0.png
|resourcenumber= SC0035
|resourcenumber= SC0035
|Learning Objectives=  
|Learning Objectives=
* recall how star distances were calculated using parallax
* recall how star distances were calculated using parallax
* explain how Christian Huygens calculated the distance of the star Sirius
* explain how Christian Huygens calculated the distance of the star
Sirius
* explain how Huygens' assumptions led to an inaccurate calculation
* explain how Huygens' assumptions led to an inaccurate calculation
* how we use black body radiation to calculate the temperature of distant stars
* how we use black body radiation to calculate the temperature of
distant stars
|age=Secondary
|age=Secondary
|content=In the 17th century, Christian Huygens discovered how to estimate how far away a star is. He made a series of smaller holes in a screen facing the sun, until he estimated the light was the same intensity as the star Sirius. Huygens' results were surprisingly accurate, but still wrong. This lesson follows work where students learn how parallax can be used to calculate the distance of stars, though not all. Students often believe that the earlier scientists made foolish assumptions. This series of slides may inspire you to tell the remarkable story of how we measure stars. It may help you help students to  
|content=In the 17th century, Christian Huygens discovered how to
understand the amazing stretches of imagination needed to come up with those early hypotheses.  
estimate how far away a star is. He made a series of smaller holes in
The teacher explains his slides in an audio file. He also provides a link to an black body radiation tool.  
a screen facing the sun, until he estimated the light was the same
intensity as the star Sirius. Huygens' results were surprisingly
accurate, but still wrong. This lesson follows work where students
learn how parallax can be used to calculate the distance of stars,
though not all. Students often believe that the earlier scientists
made foolish assumptions. This series of slides may inspire you to
tell the remarkable story of how we measure stars. It may help you
help students to
understand the amazing stretches of imagination needed to come up with
those early hypotheses.
The teacher explains his slides in an audio file. He also provides a
link to an black body radiation tool.
|format=
|format=
|strategy=
|strategy=
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|other=
|other=
|resources=
|resources=
* Teacher's audio explanation of how the lesson was delivered [[media:CT - Star brightness voiceover.MP3]]
* Teacher's audio explanation of how the lesson was delivered
[[media:CT - Star brightness voiceover.MP3]]
The presentation has been converted to alternative formats:
The presentation has been converted to alternative formats:
* Smartboard notebook version [[File:10 - Star Brightness, Size and Distance.notebook]]
* Smartboard notebook version
* Powerpoint version:[[File:10 - Star Brightness, Size and Distance.pptx]]
[[File:10 - Star Brightness, Size and Distance.notebook]]
* Powerpoint
version:[[File:10 - Star Brightness, Size and Distance.pptx]]
* PDF version [File:Star brightness & distance.pdf]]
* PDF version [File:Star brightness & distance.pdf]]
* Link to Blackbody Radiation Applet http://www.mhhe.com/physsci/astronomy/applets/Blackbody/frame.html
* Link to Blackbody Radiation Applet
http://www.mhhe.com/physsci/astronomy/applets/Blackbody/frame.html
}}
}}