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Thermonuclear bursts from slowly and rapidly accreting neutron stars

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Thermonuclear bursts from slowly and rapidly accreting neutron stars Manu Linares D. Chakrabarty, D. Altamirano, A. Cumming, L. Keek. V. Connaughton, P. Jenke, A ... – PowerPoint PPT presentation

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Title: Thermonuclear bursts from slowly and rapidly accreting neutron stars


1
Thermonuclear bursts from slowly and rapidly
accreting neutron stars
Manu Linares D. Chakrabarty, D. Altamirano, A.
Cumming, L. Keek. V. Connaughton, P. Jenke, A.
Camero-Arranz, A. van der Horst, et al.
50 years of Sco X-1, Boston, July 2012
2
PART I high-? bursts
Or how we finally found them, in a slowly
rotating neutron star. ? Sensitive to neutron
star spin?
PART II low-? bursts
Or how we hunt them in a systematic search and
find the first overlap between normal and
long/intermediate bursts. (Sensitive to neutron
star crust temperature)
? mass accretion rate per unit area
3
Burning regimes (a shell flash in a nutshell)
  • Unstable H burning
  • ?/?Eddlt0.01
  • Thermally unstable H burning.
  • Pure He ignition
  • 0.01lt?/?Eddlt0.04
  • He ignites in the absence of H.
  • Mixed H/He ignition
  • 0.04lt?/?Eddlt1
  • He ignites in a mix of HHe.
  • Stable HHe burning
  • ?/?Eddgt1
  • Both H and He burn stably. No bursts.

?accreted mass/time/area (Eddington-normalized
?/?Edd)
Increasing ?
Pic Horowitz Refs Woosley Taam (1976)
Fujimoto ea (1981) Taam (1981) Bildsten (1998)
Cumming Bildsten (2000) Woosley ea (2004)
4
Burning regimes (a shell flash in a nutshell)
  • Unstable H burning
  • ?/?Eddlt0.01
  • Thermally unstable H burning.
  • Pure He ignition
  • 0.01lt?/?Eddlt0.04
  • He ignites in the absence of H.
  • Mixed H/He ignition
  • 0.04lt?/?Eddlt1
  • He ignites in a mix of HHe.
  • Stable HHe burning
  • ?/?Eddgt1
  • Both H and He burn stably. No bursts.

BURST RATE INCREASES!
Increasing ?
5
Bursting regimes (observational status until 2010)
Linares et al. (2011)
Where are the bursts at ? gt 0.1 ?Edd?? Cornelisse
ea (03) in t Zand ea (07) Galloway ea (08)
6
T5X2 smooth burst evolution
50 Edd
10 Edd
RXTE PCA
11 Hz X-ray pulsar. Unprecedented smooth
evolution bursts-mHz QPO-bursts!
Did we underestimate influence of fast spin on
burning regimes?
Linares ea (2010,2011,2012) Strohmayer ea
(2010) Papitto ea (2010) Motta ea (2011)
Chakraborty Bhattacharyya (2011)
7
PART I high-? bursts
Or how we finally found them, in a slowly
rotating neutron star. ? Sensitive to neutron
star spin?
PART II low-? bursts
Or how we hunt them in a systematic search and
find the first overlap between normal and
long/intermediate bursts. (Sensitive to neutron
star crust temperature)
? mass accretion rate per unit area
8
Low-? bursts (how frequent are they?)
Low-? bursts recur on week-months timescales,
but such recurrence times are ill-constrained
using pointed observations.
9
The Fermi-GBM X-ray burst monitor
  • World English Dictionary
  • monitor   n 1. a person or piece of equipment
    that warns, checks, controls, or keeps a
    continuous record of something.
  • FoV all unocculted (75) sky.
  • X-ray response down to 8 keV.
  • ?Optimal instrument to detect rare bright X-ray
    bursts.

Systematic X-ray burst search and processing at
NSSTC MIT. So far (March 2010June 2012) 1490
XRB candidates (1.8/day).
10
GBM thermonuclear bursts 4U061409
15 GBM bursts from 4U 061409 in the 1st year!
(33 bursts detected in the previous gt30 years
Kuulkers et al. 2010)
11
GBM thermonuclear bursts 4U061409
Linares et al. (2012)
Burst recurrence time in 4U 061409 (2010-2011)
12 /- 3 d Shortest burst pair ever seen from the
source 2.8 days apart.
12
GBM thermonuclear bursts 4U061409
Chenevez et al. (2008)
Does the long burst population reflect a distinct
ignition regime or a selection effect?
Burst energies in 4U 061409 overlap with normal
and long burst populations.
13
PART I high-? bursts
Summary Conclusions
  • Unprecedented burst behavior in the 11 Hz pulsar
    T5X2, in agreement with theoretical burning
    regimes.
  • Three bursting regimes when mdot increased 10-50
    Edd marginally stable burning, mHz QPOs.
  • ? Are burning regimes sensitive to neutron star
    spin?

PART II low-? bursts
  • Burst recurrence time in 4U 061409 12 /- 3 d
    two bursts only 2.8 d apart.
  • Burst energies between those of normal and long
    bursts.
  • ? Are normal and long bursts two distinct
    populations?

14
Thanks!
Refs.
Millihertz Quasi-periodic Oscillations and
Thermonuclear Bursts from Terzan 5 A Showcase
of Burning Regimes (Linares et al. 2012, ApJ,
748, 82) The Fermi-GBM X-ray burst monitor
thermonuclear bursts from 4U 061409 (Linares et
al. 2012, ApJ, to be submitted)
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