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The fate of S-AGB stars. Why won’t my code converge?. or. Work in Progress! No answer yet!. Herbert Lau Pilar Gil Pons Carolyn Doherty Me. Overview. Numerical problem ?. Massive AGBs fail to converge when M env about 2 M ʘ. Physical problem ?. Overview. Numerical problem ?.

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the fate of s agb stars

The fate of S-AGB stars

Why won’t my code converge?

or

work in progress no answer yet
Work in Progress!No answer yet!
  • Herbert Lau
  • Pilar Gil Pons
  • Carolyn Doherty
  • Me
overview
Overview

Numericalproblem?

MassiveAGBsfailto converge whenMenvabout 2 Mʘ

Physicalproblem?

overview1
Overview

Numericalproblem?

MassiveAGBsfailto converge whenMenvabout 2 Mʘ

Physicalproblem?

L>LEdd

Extreme

lowρbelow BCE

looking at the facts when does it happen
Looking at the facts:when does it happen?

The divergence happens for different evolution codes (EVOLV, MONSTAR)

Can be delayed by increasing alpha (MLR)=>

increasing mixing efficiency (Herwig et al., Althaus et al,…)

looking at the facts when does it happen1
Looking at the facts:when does it happen?

Comparison: the last two TPs

slide7
Pg < 0
  • Code dies with negative gas pressure
  • T and P are dependent variables
    • So values chosen by matrix solution
    • Prad = 1/3aT4 then known
    • Pgas = P – Prad is known
    • Then the e.o.s. tells us r
  • So a Pg < 0 error means Prad provides all of P
  • ie b < 0 and L > LEdd
  • See Wood and Faulkner 1986!!
looking at the facts contribution p p rad in the hydrostatic case
Looking at the facts: contribution P/Prad in the hydrostatic case

Convective case:

then:

then:

with:

with:

Radiative case:

looking at the facts
Looking at the facts

Conductivity radiation-to-convection

ρ+Δρ

P+ΔP

T+ΔT

ρe, Pe, Te

U >> convectioninefficient

U << convectionefficient

ρ, P, T

ρe, Pe, Te

what pushes l l edd
What pushes L > LEdd ?

Reduce LEdd by increasing <k> ???

hypothesis peak
Hypothesis κ-peak
  • Petrovic et al (2006)
    • OPAL opacity tables display a peak due to presence of Fe, Ni at T aprox. 250000 K
    • This peak causes huge inflation and departure of hydrostatic equilibrium in WR stars
  • Could this be our case?
slide15

Testing the κ-peak hypothesis:

  • We smoothed out the peak
  • and the code keeps converging!
  • The star lost a further 0.5 Msun
  • Before it died again!.
multiple peaks
Multiple κ-peaks
  • We doubt the star can avoid its fate…
  • Deep envelope and low density mean a region of increasing opacity
  • The high luminosity drives dramatic expansion
  • In our hydrostatic case its supersonic!
    • 103 – 104 R per year!
  • What does a REAL star do?
  • We think the energy involved < binding energy of the envelope
  • But it might drive periodic, enhanced mass-loss at least?
the general picture
The general picture

extreme low ρ-high T zone

L>LEdd

Energy released after K peak

Loss of hydrostatic eq

code converges

If we avoid the K peak

Another hydrodynamic problem...