barbara ercolanobarbara ercolano university of exeter tuesday, 27 july 2010 tuesday, 27 july 2010...
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Thanks to:James Owen, C. Clarke (IoA); A. Glassgold (Berkeley);
S. Mohanty (Imperial); N. Turner (JPL); J. Drake, J. Raymond (CfA)
X-ray irradiated protoplanetary discs
Barbara Ercolano University of Exeter
Tuesday, 27 July 2010
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Tuesday, 27 July 2010
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Tuesday, 27 July 2010
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X-ray Feedback on Low Mass Star & Planet Formation
Taurus – Spitzer Space Telescope
Tuesday, 27 July 2010
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X-ray Feedback on Low Mass Star & Planet Formation
Taurus – Spitzer Space Telescope
Gued
el e
t al.,
200
7
Tuesday, 27 July 2010
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What drives the dispersal of disks? On what timescales?
What environments are favourable to the formation of terrestrial and giant planets?
What is the effect of irradiation on planetary atmospheres?
X-ray Feedback on Low Mass Star & Planet Formation
Taurus – Spitzer Space Telescope
Tuesday, 27 July 2010
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Tuesday, 27 July 2010
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Credit: NASA/LMSAL
Tuesday, 27 July 2010
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X-Rays
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X-RaysMRI
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X-Rays
Dead Zone
Proto-Earth
MRI
Tuesday, 27 July 2010
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X-Rays
Dead Zone
Proto-Earth
Proto-Jupiter
Photoevaporation
migration
MRI
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•‘Hard’ X-rays: MRI and Dead Zones
•‘Soft’ X-rays: Disc photoevaporation
Overview
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•‘Hard’ X-rays: MRI and Dead Zones
•‘Soft’ X-rays: Disc photoevaporation
Overview
‘Hard’ : E > 1 keV
‘Soft’ : 0.1 < E < 1 keV
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•‘Hard’ X-rays: MRI and Dead Zones
•‘Soft’ X-rays: Disc photoevaporation
Overview
‘Hard’ : E > 1 keV
‘Soft’ : 0.1 < E < 1 keV
Tuesday, 27 July 2010
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•MRI and Dead Zones
•Igea & Glassgold 1999
•X-rays from YSO dominate the disc ionisation structure
•Discs around solar-type stars mostly MRI active
•Dead-zone should extend to aprrox 5 AU
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•Igea & Glassgold 1999
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•Turner & Sano 2008•Turner & Drake 2009
•Dead or Undead?
•Use IG99 ionisation rates for stellar X-ray & consider other ionisation processes in the MMSN
•Dead zones basically always present
•Undead zones important?
•MRI active
•dead•undead
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•Mohanty, Ercolano & Turner 2010 in prep
•MRI & (Un)Dead Zones in YSO Discs
•New ionsation rates calcs with MOCASSIN
•Chemical network to account for recombinations on grains
•Parameter space investigation
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•Mohanty, Ercolano & Turner 2010 in prep
•MRI & (Un)Dead Zones in YSO Discs
•New ionsation rates calcs with MOCASSIN
•Chemical network to account for recombinations on grains
•Parameter space investigation
•DZ present in all discs with Md > 1% M*
•MRI is reduced for discs with small grains or low densities
•Grains play a major role in determining accretion in discs
Tuesday, 27 July 2010
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•‘Hard’ X-rays: MRI and Dead Zones
•‘Soft’ X-rays: Disc photoevaporation
Overview
‘Hard’ : E > 1 keV
‘Soft’ : 0.1 < E < 1 keV
Tuesday, 27 July 2010
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high mass
Viscous evolution predicts….
high accretion rate
time
low mass
low accretion rate
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high mass
Viscous evolution predicts….
Observations instead show….
t~106yrs t~107yrs
high accretion rate
time
low mass
low accretion rate
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high mass
Viscous evolution predicts….
Observations instead show….
t~106yrs t~107yrsRare transition disk
high accretion rate
time
low mass
low accretion rate
Tuesday, 27 July 2010
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Alexander, based on a description of viscous evolution
Viscous evolution
Ac
cr
etio
n r
ate
The Classical EUV switch modelClarke et al. (2001); Matsuyama et al. (2003);
Ruden (2004)
Time
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Alexander, based on a description of viscous evolution
Viscous evolution
Wind rate
Ac
cr
etio
n r
ate
The Classical EUV switch modelClarke et al. (2001); Matsuyama et al. (2003);
Ruden (2004)
Time
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Alexander, based on a description of viscous evolution
Viscous evolution
Wind rate
Viscous +windAc
cr
etio
n r
ate
The Classical EUV switch modelClarke et al. (2001); Matsuyama et al. (2003);
Ruden (2004)
Time
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Modelling photoevaporating disks: HOW?
Ercolano+ 2008, 2009, Owen+ 2010, Ercolano & Clarke 2010, Ercolano & Owen 2010, Owen, Ercolano & Clarke 2010
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Modelling photoevaporating disks: HOW?
1) Radiative Transfer (MOCASSIN) a) 2D (at least) b) gas (photoionisation) + dust 2) Hydrodynamics (ZEUS)
3) Viscous Evolution
Ercolano+ 2008, 2009, Owen+ 2010, Ercolano & Clarke 2010, Ercolano & Owen 2010, Owen, Ercolano & Clarke 2010
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Owen, Ercolano, Clarke & Alexander, 2010
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Owen, Ercolano, Clarke & Alexander, 2010
Total photoevaporation rate of ~1.4e-8 Msun/yr
(for Lx = 2e30erg/sec)
Comparable to accretion rates of CTTs
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Owen, Ercolano, Clarke & Alexander, 2010Tuesday, 27 July 2010
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Tuesday, 27 July 2010
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Ow
en, E
rcol
ano
& C
lark
e 20
10, i
n pr
ep
0
2
4
log(Surface Density) [g cm 3]
log(
Surfa
ce D
ensi
ty) [
g cm
3 ]
0.1 1 10 10010 11
10 10
10 9
10 8
Radius [AU]
Accr
etio
n R
ate
[M
yr1 ]
!
No photoevaporation
Photoevaporation
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Ow
en, E
rcol
ano
& C
lark
e 20
10, i
n pr
ep
0
2
4
log(Surface Density) [g cm 3]
log(
Surfa
ce D
ensi
ty) [
g cm
3 ]
0.1 1 10 10010 11
10 10
10 9
10 8
Radius [AU]
Accr
etio
n R
ate
[M
yr1 ]
!
No photoevaporation
Photoevaporation
Photoevaporation-starved accretion?
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Why do non-accreting YSOs (WTTs) have higher LX than accreting YSOs (CTTs) ??
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Accretion ‘disturbs’ X-ray emission
(e.g. Flaccomio et al 2003, Stassun et al 2004, Preibisch et al 2005, Jardine et al 2006, Guedel et sl 2007, Gregory et al 2007)
Why do non-accreting YSOs (WTTs) have higher LX than accreting YSOs (CTTs) ??
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Accretion ‘disturbs’ X-ray emission
(e.g. Flaccomio et al 2003, Stassun et al 2004, Preibisch et al 2005, Jardine et al 2006, Guedel et sl 2007, Gregory et al 2007)
Why do non-accreting YSOs (WTTs) have higher LX than accreting YSOs (CTTs) ??
X-rays modulate accretion?X-ray photoevaporation-starved accretion
(Drake et al 2009)
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Drake et al 2009
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Ow
en, E
rcol
ano
& C
lark
e 20
10, i
n pr
ep
0 2 4 6 8 10 121028
1029
1030
1031
Time [Myr]
Xra
y Lu
min
osity
[erg
s1 ]
WTTs (discless)
CTTs (discbearing)
Data points from Taurus (Guedel et al 2007)
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Ow
en, E
rcol
ano
& C
lark
e 20
10, i
n pr
ep
10.5 10 9.5 9 8.5 8 7.5 7
log(Accretion Rate) [M yr 1]
29
29.5
30
30.5
31
11 10.5 10 9.5 9 8.5 8 7.528.5
29
29.5
30
30.5
log(
Xra
y Lu
min
osity
) [er
g s
1 ]
!Log(Accretion Rate) [Msun/yr]
Log(
X-r
ay L
umin
osity
) [e
rg/s
ec]
0.5-3.5 Myr 1.5-4.5 Myr
4-8 Myr integrated lifetime
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Conclusions
X-rays control the evolution & dispersal of protoplanetary discs
& affect planet formation through:
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•Ionising the discs thus allowing MRI to work•(‘hard’ x-ray)
•Driving a photoevaporative wind that erodes the disc from the inside-out•(‘soft’ X-ray)
•(Possibly) modulating accretion through photoevaporation-starved accretion•(‘soft’ X-ray)
Conclusions
X-rays control the evolution & dispersal of protoplanetary discs
& affect planet formation through:
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Thank You!
Tuesday, 27 July 2010