'Supernova explosions' diaporamas de présentation

Chapter 3 The Science of Astronomy

Chapter 3 The Science of Astronomy. 3.1 The Ancient Roots of Science. Our goals for learning:. In what ways do all humans employ scientific thinking? How did astronomical observations benefit ancient societies? What did ancient civilizations achieve in astronomy?.

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Announcements

Announcements. Reading for next class: Chapter 20 Cosmos Assignment 2, Due Wednesday, April 14 Angel Quiz. Questions:. Black Holes Star-Gas-Star cycle Halo, halo stars, halo vs. bulge, halo vs disk Spiral arms Do dying stars come back as the same star? superbubbles. Halo Stars:

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Hubble Science Briefing

Hubble Science Briefing. 30 Doradus: Birthplace of giants and dwarfs. Elena Sabbi. June 7, 2012. Outline. How stars form and evolve; How we can use star clusters to better understand high redshift galaxies; Characteristics of the Large Magellanic Cloud;

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Supernovae

Supernovae. Padi Boyd.

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Opportunities for synthesis of new superheavy nuclei (What really can be done within the next few years)

Opportunities for synthesis of new superheavy nuclei (What really can be done within the next few years). State of the art Outline of the model (4 slides only) Our predictions and proposals: Elements 119 and 120 are coming

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Stellar Explosions

Stellar Explosions. Introduction. Life after Death for White Dwarfs The End of a High-Mass Star Supernovae Supernova 1987A The Crab Nebula in Motion The Formation of the Elements The Cycle of Stellar Evolution. Life after Death for White Dwarfs.

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Abundances of Isotopes from nuclear line spectroscopy

Abundances of Isotopes from nuclear line spectroscopy. Janina Fiehl. General facts about nuclear gamma line spectroscopy. The natural gamma radiation in the cosmos covers several orders of magnitudes in terms of their energy- roundabout 70 keV to 8 MeV.

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Announcements

Announcements. Projects are graded! Almost all were quite good--congratulations! Test next week (all about stars) Second project is due in three weeks. So many things I would have done, But clouds got in my way. --Joni Mitchell. Black Holes. 10 November 2006. Today :.

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Unit 1.2: Characteristics of Stars

Unit 1.2: Characteristics of Stars. Guiding Questions for this unit:. What two forces must be balanced for a star to achieve stability? What are the stages in the life cycle of a star? What determines whether a star will become a white dwarf, a neutron star, or a black hole?

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The Death of High Mass Stars: 8 Solar Masses and up.

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Keiichi Maeda (@MPA ? IPMU) MPA: Max-Planck-Institute for Astrophysics

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Announcements

Announcements. Radio Astronomy of Pulsars. Tiffany Pewett pewett@chara.gsu.edu. Pulsars. Remnants from supernova explosions (neutron stars). Rapidly rotating. Strong m agnetic fields. Beams of radio energy emitted at the magnetic poles. Pulsars. Pulsar Structure. Pulsar Detection.

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CH 25.5 Solar System Formation

CH 25.5 Solar System Formation . Objectives: How did our solar system form? What evidence supports our ideas?. http://atropos.as.arizona.edu/aiz/teaching/nats102/mario/solar_system.html. Nebular Theory. The solar system formed from a cloud of dust and gas (nebula). 4.6 billion years ago

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The Milky Way Galaxy

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R -process Nucleosynthesis in Supernova Explosions

R -process Nucleosynthesis in Supernova Explosions. Ryohei Fukuda 1 , Motoaki Saruwatari 1 , Masa-aki Hashimoto 1 , Shin- ichiro Fujimoto 2 1 D epartment of Physics, Kyushu University, Fukuoka 2 Department of Electronic Control, Kumamoto National College of Technology, Kumamoto.

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