Today’s Topics...Today’s Topics Wednesday, November 13, 2019 (Week 11, lecture 27) –Chapters...
Transcript of Today’s Topics...Today’s Topics Wednesday, November 13, 2019 (Week 11, lecture 27) –Chapters...
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Today’s TopicsWednesday, November 13, 2019 (Week 11, lecture 27) – Chapters 17, 18, 19, 22.
1. Solar fusion
1. Overview of common stars
2. Luminosity vs mass
3. H-R diagram: main sequence stars
Reminder: Midterm on Monday, November 18, 2019.
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Solar Fusion: proton-proton chain
By Sarang - Own work, Public Domain,
https://commons.wikimedia.org/w/index.php?curid=51118538
2 1.442 MeV
2 5.49 MeV+
12.86 MeV+
= 26.7 MeV total
= 4.28 10-12 J
9 billions years
weak force
4 seconds
strong force
400 years
strong force
(Note: 1 eV = 1.602 10-19 J)
(see also Sept. 20
lecture)
2 (0.42 + 2 0.511) MeV
𝑒+𝑒+
𝒆+ mass
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Einstein: Mass & Energy
𝐸𝑛𝑒𝑟𝑔𝑦 = 𝐸 = 𝑚𝑐2
massc = speed of light
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Einstein: Mass & Energy
𝐸𝑛𝑒𝑟𝑔𝑦 = 𝐸 = 𝑚𝑐2
massc = speed of light
Example: Mass converted to energy in p-p fusion
𝑚 =𝐸
𝑐2=
4.28×10−12
(3×108)2= 4.76 × 10−29 kg
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Einstein: Mass & Energy
𝐸𝑛𝑒𝑟𝑔𝑦 = 𝐸 = 𝑚𝑐2
massc = speed of light
Example: Mass converted to energy in p-p fusion
𝑚 =𝐸
𝑐2=
4.28×10−12
(3×108)2= 4.76 × 10−29 kg = 2.8 % of the mass of proton
Mass of a proton: 𝑚𝑝 = 1.6726 × 10−27 kg
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Einstein: Mass & Energy
𝐸𝑛𝑒𝑟𝑔𝑦 = 𝐸 = 𝑚𝑐2
massc = speed of light
Example: Mass converted to energy in p-p fusion
𝑚 =𝐸
𝑐2=
4.28×10−12
(3×108)2= 4.76 × 10−29 kg = 2.8 % of the mass of proton
Mass of a proton: 𝑚𝑝 = 1.6726 × 10−27 kg
Mass of 4 protons: 4 ×𝑚𝑝 = 6.6905 × 10−27 kg
= 0.7 % of the mass of 4 protons
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Einstein: Mass & Energy
𝐸𝑛𝑒𝑟𝑔𝑦 = 𝐸 = 𝑚𝑐2
massc = speed of light
Example: Mass converted to energy in p-p fusion
𝑚 =𝐸
𝑐2=
4.28×10−12
(3×108)2= 4.76 × 10−29 kg = 2.8 % of the mass of proton
Mass of a proton: 𝑚𝑝 = 1.6726 × 10−27 kg
Mass of 4 protons: 4 ×𝑚𝑝 = 6.6905 × 10−27 kg
= 0.7 % of the mass of 4 protons
Mass of 4He nucleus: 𝑚𝐻𝑒 = 6.6447 × 10−27 kg
Note:
4𝑚𝑝 −𝑚𝐻𝑒 = 4.65 × 10−29 kg
difference is due to two positrons !
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By Hubble European Space AgencyCredit: Akira Fujii - http://www.spacetelescope.org/images/heic0206j/ (watermark was cropped), Public Domain, https://commons.wikimedia.org/w/index.php?curid=5246351
Observing the Stars
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By Hubble European Space AgencyCredit: Akira Fujii - http://www.spacetelescope.org/images/heic0206j/ (watermark was cropped), Public Domain, https://commons.wikimedia.org/w/index.php?curid=5246351
Orionconstellation
Observing the Stars
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By Hubble European Space AgencyCredit: Akira Fujii - http://www.spacetelescope.org/images/heic0206j/ (watermark was cropped), Public Domain, https://commons.wikimedia.org/w/index.php?curid=5246351
Procyonmag: 0.3
Siriusmag: -1.5
Betelgeusemag: 0.5 Bellatrix
mag: 1.6
Rigelmag: 0.1
Observing the Stars
Orionconstellation
Saiphmag: 2.1
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Apparent MagnitudeLogarithmic brightness scale
[OpenStax: Astronomy]
fainterbrighter
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Apparent MagnitudeLogarithmic brightness scale
[OpenStax: Astronomy]
Human eyes are logarithmic detectors of brightness, so they measure magnitude.
Apparent brightness is proportional to optical energy/power incident on detector/eye.
fainterbrighter
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Apparent MagnitudeLogarithmic brightness scale
[OpenStax: Astronomy]
Human eyes are logarithmic detectors of brightness, so they measure magnitude.
Apparent brightness is proportional to optical energy/power incident on detector/eye.
fainterbrighter
magnitude = m1-m2 = 1 corresponds to a factor of 2.512 change in brightness
∆𝑏𝑟𝑖𝑔ℎ𝑡𝑛𝑒𝑠𝑠 =𝑏2𝑏1
= 2.512∆𝑚 = 2.512(𝑚1−𝑚2)
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By Hubble European Space AgencyCredit: Akira Fujii - http://www.spacetelescope.org/images/heic0206j/ (watermark was cropped), Public Domain, https://commons.wikimedia.org/w/index.php?curid=5246351
Procyonmag: 0.3 11.5 ly
Siriusmag: -1.5 8.6 ly
Betelgeusemag: 0.5 640 ly
Bellatrixmag: 1.6250 ly
Rigelmag: 0.1860 ly
Observing the Stars
Orionconstellation
Saiphmag: 2.1650 ly
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Apparent Brightness vs Luminosity
Luminosity (definition)
Total power output of a star.
Distance of Star: The farther away a star is, the dimmer it will appear.
energy per second
[By NASA, ESA, H. Bond (STScI), and M. Barstow (University of Leicester)]
Sirius
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Apparent Brightness vs Luminosity
Luminosity (definition)
Total power output of a star.
Distance of Star: The farther away a star is, the dimmer it will appear.
Dim StarsA star may appear dim because it has low luminosity, or/and because it is further away.
Bright StarsA star may appear bright because it has high luminosity, or/and because it is closer to us.
𝑎𝑝𝑝𝑎𝑟𝑒𝑛𝑡 𝑏𝑟𝑖𝑔ℎ𝑡𝑛𝑒𝑠𝑠 ∝𝐿𝑢𝑚𝑖𝑛𝑜𝑠𝑖𝑡𝑦
𝑑𝑖𝑠𝑡𝑎𝑛𝑐𝑒2
energy per second
[By NASA, ESA, H. Bond (STScI), and M. Barstow (University of Leicester)]
Sirius
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By Hubble European Space AgencyCredit: Akira Fujii - http://www.spacetelescope.org/images/heic0206j/ (watermark was cropped), Public Domain, https://commons.wikimedia.org/w/index.php?curid=5246351
ProcyonWhite-ish
SiriusWhite-blue
BetelgeuseRed-orange
BellatrixBlue-ish
RigelWhite-blue
Star Color
Orionconstellation
SaiphWhite-blue
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Star Color = Temperature
[OpenStax: Astronomy]
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Star Color = Temperature
[OpenStax: Astronomy]
Star light is blackbody radiation
Star color follows roughly from Wien’s law for peak wavelength: 𝜆𝑚𝑎𝑥, 𝑛𝑚 =2.9 × 106
𝑇
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Star Color = Temperature
[OpenStax: Astronomy]
Star light is blackbody radiation
Star color follows roughly from Wien’s law for peak wavelength: 𝜆𝑚𝑎𝑥, 𝑛𝑚 =2.9 × 106
𝑇
[astronomytrek.com/star-facts-spica]
Spica: T 25,000 K[Wikipedia: Stephen Rahn]
Vega: T 10,000 K CentauriT 6,000 K
[Wikipedia: Skatebiker]
AldebaranT 4,000 K
[Wikipedia: Giuseppe Donatiello]
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Luminosity = Output Power
Stellar luminosity is given by
𝐿𝑢𝑚𝑖𝑛𝑜𝑠𝑖𝑡𝑦 = 𝑂𝑢𝑡𝑝𝑢𝑡 𝑃𝑜𝑤𝑒𝑟 = 𝐼𝑛𝑡𝑒𝑛𝑠𝑖𝑡𝑦 × 𝑆𝑢𝑟𝑓𝑎𝑐𝑒 𝐴𝑟𝑒𝑎
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Luminosity = Output Power
Stellar luminosity is given by
𝐿𝑢𝑚𝑖𝑛𝑜𝑠𝑖𝑡𝑦 = 𝑂𝑢𝑡𝑝𝑢𝑡 𝑃𝑜𝑤𝑒𝑟 = 𝐼𝑛𝑡𝑒𝑛𝑠𝑖𝑡𝑦 × 𝑆𝑢𝑟𝑓𝑎𝑐𝑒 𝐴𝑟𝑒𝑎
Light intensity for a blackbody is given by the Stefan-Boltzmann law:
𝐼𝑛𝑡𝑒𝑛𝑠𝑖𝑡𝑦 = 𝜎𝑇4
A hot star is more luminous
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Luminosity = Output Power
Stellar luminosity is given by
𝐿𝑢𝑚𝑖𝑛𝑜𝑠𝑖𝑡𝑦 = 𝑂𝑢𝑡𝑝𝑢𝑡 𝑃𝑜𝑤𝑒𝑟 = 𝐼𝑛𝑡𝑒𝑛𝑠𝑖𝑡𝑦 × 𝑆𝑢𝑟𝑓𝑎𝑐𝑒 𝐴𝑟𝑒𝑎
Light intensity for a blackbody is given by the Stefan-Boltzmann law:
𝐼𝑛𝑡𝑒𝑛𝑠𝑖𝑡𝑦 = 𝜎𝑇4
The surface area of a star is related to its radius, i.e. size:
𝑆𝑢𝑟𝑓𝑎𝑐𝑒 𝐴𝑟𝑒𝑎 = 4𝜋𝑅2
A hot star is more luminous
A large star is more luminous
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Stellar Census Stellar Statistics
Milky Way galaxy (near/short-infrared: 1.25 µm, 1.65 µm, 2.15 µm)European Southern Observatory
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By Hubble European Space AgencyCredit: Akira Fujii - http://www.spacetelescope.org/images/heic0206j/ (watermark was cropped), Public Domain, https://commons.wikimedia.org/w/index.php?curid=5246351
About Half of “Stars” are Binary/Trinary Stars
Procyon
Sirius
Betelgeuse
Bellatrix
Rigel
Orionconstellation
Saiph
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By Hubble European Space AgencyCredit: Akira Fujii - http://www.spacetelescope.org/images/heic0206j/ (watermark was cropped), Public Domain, https://commons.wikimedia.org/w/index.php?curid=5246351
About Half of “Stars” are Binary/Trinary Stars
Procyon
Sirius
Betelgeuse
Bellatrix
Rigel
Orionconstellation
Saiph
![Page 27: Today’s Topics...Today’s Topics Wednesday, November 13, 2019 (Week 11, lecture 27) –Chapters 17, 18, 19, 22. 1. Solar fusion 1. Overview of common stars 2. Luminosity vs mass](https://reader035.fdocuments.in/reader035/viewer/2022071022/5fd6a6ef223cb21cc932effa/html5/thumbnails/27.jpg)
Mass-Luminosity Relation
logarithmic scale
logarithmic scale
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Mass-Luminosity Relation
𝐿𝑢𝑚𝑖𝑛𝑜𝑠𝑖𝑡𝑦 ~ 𝑀𝑎𝑠𝑠3.9
logarithmic scale
logarithmic scale
Units: Solar Mass Msun
Units:Solar Luminosity Lsun
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Temperature-Luminosity RelationH-R diagram
(Hertsprung-Russell diagram)
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Temperature-Luminosity RelationH-R diagram
(Hertsprung-Russell diagram)
90% of stars are on “main sequence”