National Science Olympiad Astronomy C Event 2013 Stellar Evolution and Type II Supernovas

Transcription

1 National Science Olympiad Astronomy C Event 2013 Stellar Evolution and Type II Supernovas DISCLAIMER This presentation was prepared using draft rules. There may be some changes in the final copy of the rules. The rules which will be in your Coaches Manual and Student Manuals will be the official rules.

2 Chandra X-Ray Education & Public Outreach Office Donna L Young, Lead Educator donna@aavso.org Tad Komacek tkomacek@uchicago.edu

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4 ASTRONOMY, Division C DESCRIPTION: Students will demonstrate an understanding of the basic concepts of mathematics and physics relating to stellar evolution and Type II supernova events. A TEAM OF UP TO: 2 APPROXIMATE TIME: 50 minutes THE COMPETITION: Each team is permitted to bring two laptops, or two 3-ring binders, or one laptop computer and one 3-ring binder (any size) containing information in any form from any source. The materials must be 3-hole punched and inserted into the rings (notebook sleeves are allowable). Each team member is permitted to bring a programmable calculator. No Internet access is allowed.

5 Using information which may include Hertzsprung-Russell diagrams, spectra, light curves, motions, cosmological distance equations and relationships, stellar magnitudes and classification, multi-wavelength images (X-ray, UV, optical, IR, radio), charts, graphs, animations and DS9 imaging analysis software, participants will be asked to complete activities which include the following: Use all available information to determine answers relating to stellar evolution, including stellar nurseries and star formation, proto-stars, main sequence stars, Cepheid variables, semiregular variables, red supergiants, neutron stars, magnetars, pulsars, Wolf-Rayet stars, stellar mass black holes, x-ray binary systems, and Type II supernovas. Use all available information, including Kepler s laws, rotation and circular motion to determine answers relating to the orbital motions of binary and multiple star systems; use parallax, spectroscopic parallax, and the distance modulus to calculate distances to Cepheid variables. Students should be knowledgeable about the properties and characteristics of the stages of stellar evolution listed above, including spectral features and chemical composition, luminosity, blackbody radiation, color index (B-V), and H-R diagram transitions. Students will be asked to identify, know the location, be knowledgeable about, and/or answer questions relating to the three content areas outlined above for the following Objects: Cas A, IGR J17091, NGC 6888/WR 136, PSR J , Cygnus X-1, SXP 1062, M1, Delta Cep, V838 Mon, α Orionis, SN 2010JL, NGC 3582, LHa115-N19, IC 1396, Antares, the rho Ophiuchi cloud complex

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7 Deep Sky Objects: A. Stellar Nurseries & Star Formation 1) rho Ophiuchi Cloud Complex 2) IC 1396 (Elephant s Trunk Nebula) 3) NGC 3582 B. Stars 1) delta Cep Cepheid variable star 2) α Orionis (Betelgeuse) red supergiant 3) α Scorpii (Antares) red supergiant 4) V838 Mon red supergiant C. Type II Supernova remnants/cores 1) Cas A 2) SXP ) M1 (Crab Nebula) 4) LHa115-N19 5) NGC 6888/WR 136 (Crescent Nebula) 6) SN 2010JL 7) PSR J D. X-Ray Binaries 1) IGR J ) Cygnus X-1

8 Stellar Nurseries & Star Formation rho Ophiuchi Cloud Complex

9 Stellar Nurseries & Star Formation IC (Elephant s Trunk Nebula)

10 r Nurseries & Star Formation NGC 3582

11 : Delta Cep (δ Cephei)

12 δ Cephei prototype of all Cepheid variable stars epsilon 4.2 zeta 3.6 delta cep alpha 2.4 iota 3.5 beta 3.2 gamma 3.2

13 lta Cep (δ Cephei) Cepheid Instability Strip

14 : α Orionis - Betelgeuse

15 : α Scorpii Antares

16 : V838 Monocerotis

17 Semiregular Variables: Semiregular Variables

18 II Supernova: Cassiopeia A (Cas A)/ Neutron Star

19 II Supernova: SXP 1062/ Pulsar

20 II Supernova: M1 (The Crab Nebula)/ Pulsar

21 II Supernova: LHa115-N19

22 II Supernova: NGC 6888/WR 136 (Crescent Nebula) Wolf Rayet Star

23 II Supernova: SN 2010JL

24 II Supernova: PSR J / Magnetar

25 y Binary: IGR J17091/ Black Hole

26 y Binary: Cygnus X-1/ Black Hole

27 Spectroscopy n G2 Arcturus - K1 Procyon F5

28 ctral Image ctral Plot ctral Image pectral Plot

29 ctral Image pectral Plot drogen mer es ctral Image, ctral Plot & mer es

30 tra tral Plot rogen er Lines nhofer Lines a, H, He

31 Summary of the Classification of Stars Spectral Class Temperature ( o K) Strength of Balmer lines Other lines to look for O 30,000-60,000 weak or not visible Ionized He (4540Å) B 10,000-30,000 moderate A 7,500-10,000 strong F 6,000-7,500 weak Ionized Ca (3930Å, 3970Å) strong compared to neutral H (4340Å) G 5,000-6,000 weak Ionized Ca (3930Å, 3970Å) strong compared to neutral H (4340Å) K 3,500-5,000 weak or not visible Many lines, neutral Ca 4230 Å M < 3,500 not visible Many lines

32 Image Sets

33 Blackbody Radiation

34 llar Radiation Laws: anck s Law ien s Law efan-boltzmann s Law L = 4πR 2 σt 4

35 Cosmological Distances Cepheid Variables

36 Cepheid Variable Stars: od-luminosity Relationship and The Distance Modulus M v = m - 5log10 (r) 10 M sun -M* = 2.5 log L*/L sun

37 se Square Law: L = 1/r 2 mference, Area, Surface Area, and Volume of a Sphere sic Equations and Relationships istance Modulus: M = m - 5log 10 (r) 10 er s 3 rd Law: (M A + M B ) = a 3 ; a = v ; 2π a = vp ; F c = ma c ; a c = v 2 = rω 2 t r p 2 l Angle Formula: D = αd 206,265 = 206,265 au = 3.26 ly = 3.08 x m 60 arcmin = 60 ; 1 = 60 arcsec = 60

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43 vso.org

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45 dra.harvard.edu.org.nasa.gov