Presentation on theme: "Reminders Due by the end of the day: – Analysis of 10 datasets – Questions from Section 2 of Searching for and Analyzing Pulsars Tonight: I will (along."— Presentation transcript:
Reminders Due by the end of the day: – Analysis of 10 datasets – Questions from Section 2 of Searching for and Analyzing Pulsars Tonight: I will (along with Mrs. Hedrick) be grading your responses for Section 1 questions.
Bellwork Degenerate Matter and Pressure A review from yesterday Why do you think degenerate gas behaves more like a sold than the gas you are familiar with here on Earth? Discuss your predictions with your group
Q: Why do degenerate gases resist compression? A:
Q: Describe how the source of pressure in normal matter and degenerate matter differ. A: Normal MatterDegenerate matter Electromagnetic Repulsion from atoms (in the case of you and me and planet Earth) Or Thermal and radiative pressure from thermonuclear fusion (in the case of stars) Degeneracy Pressure Electron degeneracy pressure (in the case of a white dwarf star) Neutron degeneracy pressure (in the case of a neutron star) Both examples depend on the temperature of the atoms/particles in the system The pressure depends only on the degenerate electrons – if heat is added the electron pressure does not increase. Follows Ideal Gas law DOES NOT Follow Ideal Gas law
Q: What happens to the volume of a white dwarf or neutron star when mass is added onto its surface? How is this different from normal matter? A: Volume when mass is added Normal MatterIncreases Degenerate MatterDecreases
Do the pulsar masses fit the predicted models developed by Chandrasekhar and the TOV group?
The Interiors of Neutron Stars An article review
Whale of a Burst Artists conception of Magnetar Gamma Ray Burst (SGR ) Artists conception of Star Quake SWIFT Spike in gamma photons
You can get this on a T-shirt
Neutron Star Crust is Stronger than Steel Gianormous flare caused by Star Quakes!
Solid Crust – Fluid Interior Possibly small mountains on the surface – really small!
Journey to the Center of a Neutron Star Watch an animation of a glitch pulse here: gov/mpg/ main_neutron_% 20star_animation. mpg
Chemistry of a neutron star modeled for first time Gamma and X-ray emission during zombie- ism nters/goddard/mpeg/97 911main_Puff.0539.mpe g
Exploded Star Reveals Strange New Matter Cas A Supernova Remnant: g g Cas A is a young pulsar. It has slowed down tremendously over the last 10 years ~ 4%. This is believed to be due to the rapid cooling of the inside. Forming superfluid and super conductors (Resistance free material – this allows electrons to flow freely) Superfluid's on Earth: (small clip) Superfluid’s on Earth (long clip)
Now, let’s put all the information about the interior of a neutron star together and create a 2-D or 3-D model representing what we have learned. Groups of 2 or 3 You can create a 2-D model using markers Or a 3-D model using play dough Either way you must have a way to label and describe each layer