Lecture 16

Lecture 16 - • Neutron star magnetic field can control flow of ionized gas • Just like solar magnetic field can prevent convection in sunspots

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1. Size o Extremely small with extremely high mass o Remember-- granules on the sun (millions of them) are each the size of Texas o A neutron star is smaller than baton rouge and has the SAME mass as the ENTIRE sun 2. Inside a Neutron Star o Different from anything we've discussed before o Super fluid rotating around that causes a magnetic field affected by electrical currents 3. Millisecond Pulsars o Binary stars make them go faster o Point where gravity in between them balances out 4. Interacting Binaries come in many varieties o Accreting normal star (Algol in Perseus) "the winking demon" - flashed everytime the binary passed in front o Accreting white dwarf More massive star evolves and loses envelope as planetary nebula 5. X ray pulsars o Some pulsars are undetected in radio . .but emit pulsed x rays Gas tries to accrete onto neutron star
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Unformatted text preview: • Neutron star magnetic field can control flow of ionized gas • Just like solar magnetic field can prevent convection in sunspots • Also like flow of gas from earth's magnetic field and down onto poles (aurorae) • Creates xray hot spots on neutron star poles - 10 8 k! 6. Solution to the millisecond pulsar problem o Why are they spinning so fast? • Old (spinning down only slowly) • Should be slow now o Solution- they were spun up • Most MSPs have binary companions • As neutron star captures rotating gas from dish it spins it up o Some MSPs are not in binarys o Theory • Evolve from accreting pulsars • Spins the pulsar up o Prediction • We should see accreting MSPs • Missing link between accreting slow pulsars and non accreting MSPs...
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This note was uploaded on 03/30/2012 for the course ASTR 1102 taught by Professor Staff during the Spring '08 term at LSU.

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