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MASSIVE STAR FEEDBACK:CONVERGENCE BETWEEN
OBSERVATIONS AND SIMULATIONS
Eric Pellegrini, ITA, HeidelbergSILCC Collaboration
OR:WHAT’S THE CONNECTION BETWEEN
MICRO- AND MACRO-PHYSICS
Simon Glover, Ralph Klessen, Christian BaczynskiSILCC Collaboration
Macro-Physical Processing of Galaxies
SILCC – Simulating the Life Cycle
of Clouds
Simulations of stratified discs with thermal SNe
Include SNe at fixed rate (momentum and
thermal energy), Gatto+2014
Include chemical evolution (H+, H, H2, CO, C+)
Glover+2012, Walch+2014
Include shielding of the gas (attenuation of
ISRF), TreeCol (Clark+2012)
Neglect winds, direct radiation
Milky Way condistions (10 Msol/pc^2, solar Z)
Overview
Feedback
X-Ray Plasma
Thermalized
Shocks from
Stellar Winds and
Supernovae
T = 106 – 107 K
n(H) < 0.1
Radiation
Dominated by
ionizing photon
momentum
Non-Isotropic
Pressure Term-
Think Force on
Shell
HII Region Gas
Photoionized
T = 104 K
n(H) = 10 – 1000
cm-3
𝑇 = 106 K
𝑇 = 104 K
𝑇 = 101 − 102 K
Bubble Model of SF regions
M17
10/29/2015Image credit: Robert Hurt, Matthew Povich
Chandra X-ray Image
R = 8m, O=5.8 m, G=4.5 m, B=3.6 m
Basic PDR micro-Physics
Figure Credit: Kaufman, “PDR30”
Advanced H+/PDR PhysicsH
ot Sta
r(s)
H+
O++
C++
H0
O0
C+
H2
CO
depth (pc)
Isobaric EOS
Hot Sta
r(s)
H+
O++
C++
H0
O0
C+
H2
CO
MHS EOS
𝑃𝑡𝑜𝑡 𝑟 = 𝑃𝑋 + 𝑛(𝑟)𝑘𝑇 +𝐵2 𝑟
8𝜋+ 𝑃𝑡𝑢𝑟𝑏 + 𝑃𝑙𝑖𝑛𝑒𝑠 + 𝑃𝑠𝑡𝑎𝑟𝑠 𝑟
𝐵 = 𝐵0 ×𝑛
𝑛0
𝛾2
𝑇 = 106 K
𝑇 = 104 K
𝑇 = 101 − 102 K
Magneto-Hydro-Static EOS
Advanced H+/PDR PhysicsH
ot Sta
r(s)
H+
O++
C++
H0
O0
C+
H2
CO
depth (pc)
Isobaric EOS
Hot Sta
r(s)
H+
O++
C++
H0
O0
C+
H2
CO
MHS EOS
High B low n(H)
longer path length
M17
10/29/2015Image credit: Robert Hurt, Matthew Povich
Chandra X-ray Image
21cm continuum
13CO integrated
intensity
R = 8m, O=5.8 m, G=4.5 m, B=3.6 m
Brogan & Troland (2001)Pellegrini et al. (2007)
Observed SF EOS
Observed SF EOS
10/29/2015
Pre
ss
ure
D
en
sity
Observed SF EOS
10/29/2015
Pre
ss
ure
D
en
sit
y
1000
800
600
400
200
4e
7
3e
7
2e
7
1e
7
𝐵𝜇𝐺 = 59 𝑛𝑇𝑥6 + 4.8𝑄50 ℎ ҧ𝜈15
𝑅12
487𝜇𝐺
𝑅1 = 0.32𝑛𝑇𝑥6 = 3.5𝑄50 = 1.35ℎ𝜈15 = 1
Observed SF EOS
Observed SF EOS
Depth (pc)
0.0 0.1 0.2 0.3
1e+5
2e+5
3e+5
4e+5
5e+5
H+
H0
2 x H2
Enhanced CR Model
<B> = 527 G
Pre
ssu
re
(P
/k,
cm
-3 K
)
0.0
2.0e+7
4.0e+7
6.0e+7
8.0e+7
1.0e+8
Magnetic Pressure Model
<B> = 448 G
0.0
2.0e+7
4.0e+7
6.0e+7
8.0e+7
Gas Pressure Model
<B> = 0 G
Depth (pc)
0.0 0.1 0.2 0.30.0
2.0e+7
4.0e+7
6.0e+7
8.0e+7
1.0e+8
1.2e+8
gas
mag
integ rad
turb
De
nsity (
cm
-3)
0
2e+4
4e+4
6e+4
8e+4
1e+5
0
2e+4
4e+4
6e+4
8e+4
1e+5
Enhanced CR Model
<B> = 527 G
Magnetic Pressure Model
<B> = 448 G
Gas Pressure Model
<B> = 0 G
Pressure Density
Observed SF EOS
Observed SF EOSPredicted Surface Brightness
Massive Star Forming Region EOSDetailed Ionization Balance
Photoionization
Models
- Z
- Teff
- Dust
- U(n0,r0)
- EOS: n(r,T)
Nebular Emission
- H+, O++, Ar++
- O+, N+, S+
(𝑄0, 𝑇𝑒𝑓𝑓)
[𝑆 𝐼𝐼]/𝐻𝛼[𝑂
𝐼𝐼𝐼]/𝐻
𝛽
𝑟1
𝑛1 𝐻
𝑟2𝑟3
𝑃𝑟𝑎𝑑 = 𝑈 𝑟 ℎ𝜈 𝑛 𝐻
Massive Star Forming Region EOS
Massive Star Forming Region EOS
10/29/2015E. W. Pellegrini
𝑃𝑟𝑎𝑑 = 𝑈 𝑟 ℎ𝜈 𝑛 𝐻
Massive Star Forming Region EOS
10/29/2015E. W. Pellegrini
Massive Star Forming Region EOS
10/29/2015E. W. Pellegrini
Massive Star Forming Region EOS
4
3𝜋𝑟3𝑃𝑒𝑥𝑡 = 𝑀𝜎𝑣 −
𝐺𝑀2
5𝑟
Indebetow et al. 2013
Impact of SF on Molecular Clouds
30 Doradus M17 Orion-Bar
Q(H) s-1
Log R (cm)
Age (Myr)
52.0
19.8 – 22.5
25
50.0
17.9
1
49.0
17.5
≤ 0.5
𝑃𝑟𝑎𝑑𝑃𝑔𝑎𝑠
<0.1-0.4 2 0.4
𝑃𝑋𝑃𝑔𝑎𝑠
1-10 0.2 ≤ 1
𝑃𝐵𝑃𝑔𝑎𝑠
? 2 ~0.5
Feedback Summary
Convergence
“Full” 5 species chemistry
H,H2,H+,CO
Adaptive mesh ray-tracing
NLTE produces (important @IF)
ISM heating/cooling
ISRF self-shielding (Treecol)
Self-gravity
Sink Particles
Winds (Andrea Gatto)
SNe
Radiation
w/ stellar evolution
Ionization
Momentum
Convergence
“Full” 5 species chemistry
H,H2,H+,CO
Adaptive mesh ray-tracing
NLTE produces (important @IF)
ISM heating/cooling
ISRF self-shielding (Treecol)
Self-gravity
Sink Particles
Winds (Andrea Gatto)
SNe
Radiation
Ionization
Momentum
