ASTR 1040 Recitation: Mass Transfer Ryan Orvedahl Department of - - PowerPoint PPT Presentation

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ASTR 1040 Recitation: Mass Transfer Ryan Orvedahl Department of - - PowerPoint PPT Presentation

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ASTR 1040 Recitation: Mass Transfer Ryan Orvedahl Department of Astrophysical and Planetary Sciences March 17 & 19, 2014 This Week Midterms Returned Tomorrow Hooray!! Homework Due Tomorrow Hooray?? R. Orvedahl (CU Boulder) Mass

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ASTR 1040 Recitation: Mass Transfer

Ryan Orvedahl

Department of Astrophysical and Planetary Sciences

March 17 & 19, 2014

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This Week

Midterms Returned Tomorrow – Hooray!! Homework Due Tomorrow – Hooray??

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 2 / 24

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Today’s Schedule

Past / Current Homework Questions? Basics of Mass Transfer Roche Lobes Binary Systems

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 3 / 24

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Comments on Last Homework

Quickly go over last week’s homework Some stumbling points and how to get around them This may help for current homework

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 4 / 24

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Comments on Essay of Midterm II

Main sequence burning H to He

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 5 / 24

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Comments on Essay of Midterm II

Main sequence burning H to He No more H in core: core contracts, T around core ↑

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 5 / 24

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Comments on Essay of Midterm II

Main sequence burning H to He No more H in core: core contracts, T around core ↑ H around core ignites → H shell burning

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 5 / 24

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Comments on Essay of Midterm II

Main sequence burning H to He No more H in core: core contracts, T around core ↑ H around core ignites → H shell burning Core inert, still contracting, H shell dumps He onto core

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 5 / 24

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Comments on Essay of Midterm II

Main sequence burning H to He No more H in core: core contracts, T around core ↑ H around core ignites → H shell burning Core inert, still contracting, H shell dumps He onto core Temp in core rises, but not pressure (inert)

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 5 / 24

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Comments on Essay of Midterm II

Main sequence burning H to He No more H in core: core contracts, T around core ↑ H around core ignites → H shell burning Core inert, still contracting, H shell dumps He onto core Temp in core rises, but not pressure (inert) Temp rises to ∼ 100 × 106 K, He fusion in core starts

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 5 / 24

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Comments on Essay of Midterm II

No more He in core: C core contracts, T around core ↑

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 6 / 24

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Comments on Essay of Midterm II

No more He in core: C core contracts, T around core ↑ He around core ignites → He shell burning

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 6 / 24

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Comments on Essay of Midterm II

No more He in core: C core contracts, T around core ↑ He around core ignites → He shell burning Star not large enough to go any further

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 6 / 24

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Comments on Essay of Midterm II

No more He in core: C core contracts, T around core ↑ He around core ignites → He shell burning Star not large enough to go any further Vigorous shell burning, lose outer layers in gentle puffs

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 6 / 24

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Comments on Essay of Midterm II

No more He in core: C core contracts, T around core ↑ He around core ignites → He shell burning Star not large enough to go any further Vigorous shell burning, lose outer layers in gentle puffs Result: planetary nebulae and white dwarf with C core

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 6 / 24

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Lagrangian Points

Transform to the rotating frame In this frame, there is no net force on spacecraft at the Lagrange points Without transforming: combined gravity of two

  • bjects keeps spacecraft in
  • rbit
  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 7 / 24

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5 Special Points

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 8 / 24

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Only Two are Stable

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 9 / 24

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The Other Three are Unstable

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 10 / 24

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Plot Gravitational Potential

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 11 / 24

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How Is This Related To Mass Transfer?

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 12 / 24

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How Is This Related To Mass Transfer?

Inner Lagrange point is unstable ...

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 12 / 24

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How Is This Related To Mass Transfer?

Inner Lagrange point is unstable ... What happens if a star in a binary becomes a Red Giant?

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 12 / 24

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How Is This Related To Mass Transfer?

Inner Lagrange point is unstable ... What happens if a star in a binary becomes a Red Giant? Mass Transfer!!

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 12 / 24

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Roch Lobe Overflow

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 13 / 24

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Algol Paradox

Binary system ⇒ assume stars formed at same time

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 14 / 24

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Algol Paradox

Binary system ⇒ assume stars formed at same time Massive stars evolve quicker: tMS ∼ M−3

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 14 / 24

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Algol Paradox

Binary system ⇒ assume stars formed at same time Massive stars evolve quicker: tMS ∼ M−3 Observe Algol A on main sequence and Algol B as a subgiant star

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 14 / 24

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Algol Paradox

Binary system ⇒ assume stars formed at same time Massive stars evolve quicker: tMS ∼ M−3 Observe Algol A on main sequence and Algol B as a subgiant star Algol A is more massive then Algol B Paradox??

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 14 / 24

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Algol Paradox – Not Really a Paradox

Algol A (more massive) is on main sequence Algol B (less massive) is subgiant Suppose initially: MB = 3 M⊙ and MA = 1 M⊙

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 15 / 24

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Algol Paradox – Not Really a Paradox

Algol A (more massive) is on main sequence Algol B (less massive) is subgiant Suppose initially: MB = 3 M⊙ and MA = 1 M⊙ Algol B evolved first, becomes subgiant (R ↑)

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 15 / 24

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Algol Paradox – Not Really a Paradox

Algol A (more massive) is on main sequence Algol B (less massive) is subgiant Suppose initially: MB = 3 M⊙ and MA = 1 M⊙ Algol B evolved first, becomes subgiant (R ↑) Algol B overflows its Roche Lobe ⇒ mass transfer, now closer to MA ≈ MB ≈ 2 M⊙

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 15 / 24

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Algol Paradox – Not Really a Paradox

Algol A (more massive) is on main sequence Algol B (less massive) is subgiant Suppose initially: MB = 3 M⊙ and MA = 1 M⊙ Algol B evolved first, becomes subgiant (R ↑) Algol B overflows its Roche Lobe ⇒ mass transfer, now closer to MA ≈ MB ≈ 2 M⊙ As more mass transfers, MA ≈ 3 M⊙ & MB ≈ 1 M⊙, while Algol A = MS, Algol B = subgiant

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 15 / 24

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Binary Stars That Go Boom – Type Ia

Binary system with two different mass stars Massive one evolves first, transfers mass, mass ratio switches Massive star becomes white dwarf, no longer transfers mass Other star evolves, overflows its Roche Lobe, transfers mass onto WD If accretion rate is high enough, can ignite carbon fusion and star explodes

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 16 / 24

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Simulating Stars That Go Boom – Type Ia

Step 1: flame reaches the surface

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 17 / 24

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Simulating Stars That Go Boom – Type Ia

Step 2: flame travels along the surface, think water waves

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 18 / 24

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Simulating Stars That Go Boom – Type Ia

Step 3: the surface waves compress material at the other pole

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 19 / 24

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Binary Stars That Go Boom – Novae

Evolution is the same as supernova (up to a point) End up with a white dwarf and a subgiant star that transfers mass to WD Accretion rate is smaller then SNe case Mass piles on WD in a slow manner, only enough to ignite H/He on surface Surface explosions, sometimes more then one

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 20 / 24

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Binary Stars That Go Boom – Novae

Zoomed in on left, regular field of view in right

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 21 / 24

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Binary Stars That Go Boom – Other Possibilities

Could have a neutron star - regular star systems Could have a black hole - regular star systems Could have a neutron star - neutron star systems Could have a neutron star - black hole systems Could have a black hole - black hole systems

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 22 / 24

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Do We See These Systems?

Black Hole: Cygnus X-1

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 23 / 24

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Do We See These Systems?

Neutron Star: Hercules X-1

  • R. Orvedahl (CU Boulder)

Mass Transfer Mar 17 & 19 24 / 24