Backflows in AGNs - Roma Tre Universitywebusers.fis.uniroma3.it/~agn10/file/antonuccio.pdfV. A.-D. ,...
Transcript of Backflows in AGNs - Roma Tre Universitywebusers.fis.uniroma3.it/~agn10/file/antonuccio.pdfV. A.-D. ,...
![Page 1: Backflows in AGNs - Roma Tre Universitywebusers.fis.uniroma3.it/~agn10/file/antonuccio.pdfV. A.-D. , U. Becciani INAF-Catania J. Silk Johns Hopkins/Univ. P.M. Curie S. Cielo MPIA,](https://reader036.fdocuments.us/reader036/viewer/2022071504/6124596c7a22164da7799a2d/html5/thumbnails/1.jpg)
AGN10 - University Rome 3, September 13, 2012
Backflows in AGNsBackflows in AGNs Selfregulation of accretion and of jet emission Selfregulation of accretion and of jet emission
V. A.-D. , U. Becciani INAF-CataniaJ. Silk Johns Hopkins/Univ. P.M. CurieS. Cielo MPIA, Heidelberg (made also the movies!)C. Tortora ETHA. Macciò MPIA, HeidelbergC. Norman Johns HopkinsA. Babul Univ. Victoria
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AGN10 - University Rome 3, September 13, 2012
Backflows in AGNsBackflows in AGNs Selfregulation of accretion and of jet emission Selfregulation of accretion and of jet emission
V. A.-D. , U. Becciani INAF-CataniaJ. Silk Johns Hopkins/Univ. P.M. CurieS. Cielo MPIA, Heidelberg (made also the movies!)C. Tortora ETHA. Macciò MPIA, HeidelbergC. Norman Johns HopkinsA. Babul Univ. Victoria
V. A.-D. & Silk, MN 389, 1750 (2008)Tortora et al., MN 396, 61 (2009)V. A.-D. & Silk, MN 405, 1303 (2010)Tortora et al., MN 411, 627 (2011)Crockett et al., MN 412, 1603 (2012)Silk et al., arxiv1209.1175
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Mizuta et al. (ApJ 709, L83, 2010): 2D simulations of relativistic jets Backflows along relativistic jets V. A.D. & Silk (MN 405, 1303, 2010): 2D simuls. of jetprop. inrealistic E's models With cooling and BH's radiation field
Backflows: theory
Neumeyer et al. (ApJ 671, 1329, 2007): SiVI line within ~ 100 pc of Cen A – Redshifted gas in NE part
Backflows: observations
HI SiVI 5GHz
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Laing and Bridle (MN 424, 1149, 2012): Counterflows detected in 2 FRI's – V
bck ~ 700 km/sec (5” ~ 3.7 kpc)
Counter jet gas streaming along the bow shock
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Jet/cocoon system, Tcoc
10≃ 94×1011 K, ncoc
10≃ 4101 cm3
Bow shock+contact discontinuity – Hot spot at jet termination
Dynamics of jet propagation into host galaxy
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AGN10 - University Rome 3, September 13, 2012
Jet/cocoon system, ncoc
Tcoc
n≃bs
Tbs
≫ nenv
Tenv
expands (selfsimilar model: Falle, 1991) Does not determine neither morphology nor internal flows
Dynamics of jet propagation into host galaxy
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AGN10 - University Rome 3, September 13, 2012
How does the cocoon expand?
Shearing gas gains angular momentum when crossing a gradient in h
0 (specific stagnation enthalpy) near the meridional spots
and the hotspot .
A hotspot develops near the jet's termination
A high density region develops in two spots near the meridional plane
Backflow from the HS is expected from Crocco theorem
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Backflows can provide ~ 103 – 1 M
⊙ yr1 over ~
107 yrs. Selffeeding AGN(V. A.D. & Silk, 2010)
Backflows can feed the AGN
2D Simulations: 2 modes of backflow
Early: circulation Late: counterjet
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No meridional circulation along the bow shock → flow is directly reflected from the hotspot
Similar velocity field in simulations of heavy (
j/
ism = 10-1),
adiabatic, relativistic simulations
Mizuta et al., ApJ 709, 1083 (2010)
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3D simulations of jet propagation
FLASH 3.3, Adapt. Mesh Refin.
Rad. cooling, Z=0.5 Z⊙ , incl. pair prod.(102 ≤T ≤1012 K)
8 ref. Levels, Lb = 80 kpc,
lmin
= 78.125 pc
Rad. field from the central BH (heating)
Same parameters as inV.A.D & Silk 2010 (2D)
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3D simulations of jet propagation
FLASH 3.3, Adapt. Mesh Refin. DM halo: σ
v = 150 – 250 km/sec, NFW profile
Hot ISM: T = 107 K, Ωb = 0.013 , truncated isothermal distribution
Jet/ISM/Halo/BH: parameters determined by observed scaling distributions (as in V.A.D & Silk, 2010)
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Initial setup:Scaling relations between M
BH, P
jet,
0|ism
DM halo virial mass Mv ∝
2002.99±0.15 (Lintott, Ferreras &
Lahav, 2006)
MBH
= (1.2±0.2)108 200
3.57±0.15 M⊙(Ferrarese & Merritt 2000)
log(Pjet
) = 0.22 + 0.59log(MBH
) + 40.48 (cgs, Liu, Jiang and Gu
2006)
Diffuse Interstellar Medium: embed an isothermal halo in (appr.) equilibrium within the host NFW halo (central density
0|ism,
Hester, 2006)
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Northwest: backflow (v opposite to jet) ➸ green/yellow/red Southeast: contours trace jet
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Southeast: backflow (v opposite to jet) ➸ red/yellow/green Northwest: contours trace jet
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Circumnuclear disc from early backflow
Lobe's expansion drives matter towards the meridional plane
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Formation of a circumnuclear disc
A circumnuclear, high density gaseous disc forms from the combination of backflow and compression from the lobes
t=4.624× 106t=6.172× 106t=1.54× 106
Circumnuclear discs are very frequent in nearby Ellipticals (Kawata, Cen and Ho, 2007; Davies et al., 2007)CN discs can thus arise also in absence of mergers, due to the cocoon dynamics
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AGN10 - University Rome 3, September 13, 2012
Formation of a circumnuclear disc
A circumnuclear, high density gaseous disc forms from the combination of backflow and compression from the lobes
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Enhanced SF within circumnuclear discs
NGC 7469
1'' = 80 pc
HCN gas around AGNs' nuclei (Hsieh et al., 2008; Kohno et al., 2008) Scales larger than Davies et al.: ~ 500 pc Line ratios:
RHCN/CO = 0.39
RHCN/HCO+ = 1.9 enhanced SF?
Excess gas around the circumnucl. region accreting gas, in excessof hydr. equil. (Hsieh et al. 2008) This gas can only be accounted
for if it is accreting from a larger region
Evidence for backflowing gas within the cocoon
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What controls cocoon's morphology?
Both runs:P
j = 1045 erg/sec, M
gas ≃ 2.34×1011 M
⊙, T
g = 107 K
In which parameter do they differ?
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AGN10 - University Rome 3, September 13, 2012
What controls cocoon's morphology?
Both runs:P
j = 1045 erg/sec, M
gas ≃ 2.34×1011 M
⊙, T
g = 107 K
hhjj= 4.56= 4.56××101066 erg cmerg cm33
hj = e + p + v2/2 stagnation enthalpy
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AGN10 - University Rome 3, September 13, 2012
What controls cocoon's morphology?
Both runs:P
j = 1045 erg/sec, M
gas ≃ 2.34×1011 M
⊙, T
g = 107 K
FRI morphology low internal enthalpy Diagnostics of the accretion/BAL region
hhjj= 4.56= 4.56××101066 hh
jj= 4.56= 4.56××101022
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A possible explanation of the Lbol/LEdd – age connection
Davies et al. (2007): older starburst are associated with brighter AGNs
Model: high Pj higher p
bck
faster suppression of SF in the disc
AND higher Tdisc
higher Lbol
Detailed modelling of gas+stellar discs with external backflow
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VHE γ's from Hot Spot
T > 1011 K, nhs
~ 10-3 – 10-1 cm-3
Future work
Toetota et al., et al., MNRAS 417, 2789 (2011)
Cold, star-forming cloudsFeedback: positive vs. negative
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Morphology of FRI radio galaxiesMorphology of FRI radio galaxies
0206+35''
NGC193
Laing et al., MNRAS 417, 2789 (2011)
Pj = 1045 erg/sec
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Backflows: 2D vs. 3D
2D: T~2×107 yrs., independent of central density
3D: early inflow phase (T~105 yrs.), indep. of central density
MMass flow around a 20pc sphere centred on the BHass flow around a 20pc sphere centred on the BH
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Effects of backflow on CN/accr. discs:
Stores Lz ~ 0 gas into the
accr. disc higher Pj
High enthalpy gas enhanced
circumnuclear SF
Backflow and the circumnuclear disk
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AGN10 - University Rome 3, September 13, 2012
Effects of backflow on CN/accr. discs:
Stores Lz ~ 0 gas into the
accr. disc higher Pj
High enthalpy gas enhanced
circumnuclear SF
Backflow and the circumnuclear disk
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Morphology of FRI radio galaxies
Laing et al., MNRAS 417, 2789 (2011)
M84,
Jets are relativistic (>0.92), even far away (~few kpc) from the BH
0755+37, 4''/1.3''
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Morphology of FRI radio galaxies
M84, 4''/1.3''
Jets are relativistic (>0.92), even far away (~few kpcs) from the BH
P ~ , spectral index
steepens ⊥ jet (MFs)
0755+37, 4''/1.3''
Laing et al., MNRAS 417, 2789 (2011)
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AGN10 - University Rome 3, September 13, 2012
Morphology of FRI radio galaxies
M84, 4''/1.3''
Jets are relativistic (>0.92), even far away (~few kpcs) from the BH
P ~ , spectral index
steepens ⊥ jet (MFs)
0755+37, 4''/1.3''
flat along the jet, and clumpy (jetcold clouds interactions?)
Laing et al., MNRAS 417, 2789 (2011)
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Relativistic jet propagating into the ISM: <nRelativistic jet propagating into the ISM: <nee> ~10> ~10331 cm1 cm33,,
T ~ 10T ~ 10882*102*101111 K K cocooncocoon V. A.-D. and J. Silk, MN 389, 1750 (2008)
Global expansion: Global expansion: selfsimilar, rselfsimilar, r
hshs ~ t ~ t2/52/5
(Falle, 1991)(Falle, 1991)
rrhshs
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Relativistic jet propagating into the ISM: <nRelativistic jet propagating into the ISM: <nee> ~10> ~10331 cm1 cm33,,
T ~ 10T ~ 10882*102*101111 K K cocooncocoon V. A.-D. and J. Silk, MN 389, 1750 (2008)
Global expansion: Global expansion: selfsimilar, rselfsimilar, r
hshs ~ t ~ t2/52/5
(Falle, 1991)(Falle, 1991)
A A global circulationglobal circulation arises within the cocoon,arises within the cocoon, with a regular flow with a regular flow along the bow shock along the bow shock
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lateral flow
v = 100, t=6.8x106 yrs.
∇h0
∇h0
recoll. shock
A global backflow circulation develops – abt. ~ 210*103 of the jet's gas flows back towards the BH
Adaptive Mesh refinement 2D simulations
A.D. & Silk, MN 405, 1303 (2010)
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At t~1.6x107 yrs. the recoll. shock is destroyed the meridional circulation disappears
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If Pjet
exceeds by 2 the fiducial value the backflow disappears
Pjet
= 2.31045 erg s1 in model sm200av(V. A.D. & Silk,2010)
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AGN10 - University Rome 3, September 13, 2012
If Pjet
exceeds by 2 the fiducial value the backflow disappears
Pjet
= 2.31045 erg s1 in model sm200av(V. A.D. & Silk,2010)
The environment “seen” by the relativistic jet when it first enters ISM has an impact on the global structure of the cocoon
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AGN10 - University Rome 3, September 13, 2012
dM/dt ~ 0.32 – 0.76 Msun yr1, peak values ~ 0.6 – 1.3 Msun yr1
~ 24x107 yrs. Accr. rates needed: 105 Msun yr1
Mass backflow in a 10 pc circumnuclear region
For given Pj, nism strongly affects mass flow rates and backflow energeticscompression starburst
NOTE: the backflow contributes Lz ~0
gas
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AGN10 - University Rome 3, September 13, 2012
Feedback of the backflow ON the circumnuclear disk
Effects of feedback from backflow:
Stores more Lz ~ 0 gas into the
accr. disc higher Pj
Line indices: shocks + starbursts (Mazzuca et al., 2006; Sarzi et al., 2007)
Enhanced SF from compression IntermittencySeries of SF episodes
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AGN10 - University Rome 3, September 13, 2012
Morphology of the cocoon in simulations is seen to depend on
jet's lightness ( j/
ism ), or equivalently the ratio h
j/p
ism
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AGN10 - University Rome 3, September 13, 2012
Morphology of the cocoon in simulations is seen to depend on
jet's lightness ( j/
ism ), or equivalently the ratio h
j/p
ism
Thermalization of the jet with the environment can modify hj
Most likely, a rel. jet “sees” a clumpy, two-phase ISM medium
when it emerges from the accr. disc
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AGN10 - University Rome 3, September 13, 2012
Morphology of the cocoon in simulations is seen to depend on
jet's lightness ( j/
ism ), or equivalently the ratio h
j/p
ism
Thermalization of the jet with the environment can modify hj
Most likely, a rel. jet “sees” a clumpy, two-phase ISM medium
when it emerges from the accr. disc
Jet-clouds interaction can modify also the cocoon
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AGN10 - University Rome 3, September 13, 2012
Thermal energy of the cocoon can be utilized in evaporating cold, star-forming clouds SF feedback Tortora et al., MN 396, 61 (2009)
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AGN10 - University Rome 3, September 13, 2012
Thermal energy of the cocoon can be utilized in evaporating cold, star-forming clouds SF feedback Tortora et al., MN 396, 61 (2009)
SFR is damped, AFTER an initial enhancement (positive feedback)
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AGN10 - University Rome 3, September 13, 2012
Morphology of the cocoon in simulations is seen to depend on
jet's lightness ( j/
ism ), or equivalently the ratio h
j/p
ism
Thermalization of the jet with the environment can modify hj
Most likely, a rel. jet “sees” a clumpy, two-phase ISM medium
when it emerges from the accr. disc
Jet-clouds interaction can modify also the cocoon
Thermalization of the jet affects the evolution of the cocoon
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AGN10 - University Rome 3, September 13, 2012
Thermodynamics of a relativistic jet
Rel. jet-ISM/stars interactions: Relativistic Thermodynamics How does T transform in Special Relativity? Ans: depends on the thermometer (Touschek, 1968; Israel, 1986; van Kampen, 1974, ....) Non ideal relativistic fluid: Tab explicitly includes thermal conduction (Eckart, 1974):
where:
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AGN10 - University Rome 3, September 13, 2012
Thermodynamics of a relativistic jet (contd.)
Here qa is the thermal conduction 4-vector ( qaua=0)
Relation with T (Vàn, arxiv:0712.1437, eq. 26):
where:
Rel. thermal conduction law:
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AGN10 - University Rome 3, September 13, 2012
Thermodynamics of a relativistic jet (contd.)
Define
Energy-momentum conservation:
We get:
Note that:
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AGN10 - University Rome 3, September 13, 2012
Thermodynamics of a relativistic jet (contd.)
Thus:
Jet flow line interacting with a cloud in pressure equilibrium:
pj=p
c, thus:
We get:
From here, imposing the thermal equilibrium condition between
Jet an cloud, we get: Tj T
c
If instead the jet is in eq. With a photon gas (hot stellar corona
we get (Israel, 1982): Tj T
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AGN10 - University Rome 3, September 13, 2012
Thermodynamics of a relativistic jet (end)
Thus, the temperature structure of a jet emerging from the BH is strongly affected by the local environment within the firstfew pcs of the AGN
Detailed modeling requires also to take into account the effects of the backflow on the thermal structure of the jet
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AGN10 - University Rome 3, September 13, 2012
Conclusion The thermal structure (enthalpy, lightness) of a relativistic AGN jet is important to determine the structure/morphology of thecocoon
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AGN10 - University Rome 3, September 13, 2012
Conclusion The thermal structure (enthalpy, lightness) of a relativistic AGN jet is important to determine the structure/morphology of thecocoon Unknown composition of the jet can be constrained by a relativistic thermodynamic of the jet-cloud-coronae interaction
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AGN10 - University Rome 3, September 13, 2012
Conclusion The thermal structure (enthalpy, lightness) of a relativistic AGN jet is important to determine the structure/morphology of thecocoon Unknown composition of the jet can be constrained by a relativistic thermodynamic of the jet-cloud-coronae interaction At higher z (~1-4) more gas-rich AGN hosts, thus the impact of jet's thermalization is potentially higher than in the nearby Universe
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AGN10 - University Rome 3, September 13, 2012
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AGN10 - University Rome 3, September 13, 2012
1'' = 80 pc
Evidence for stellar discs on scales 1100 pc in Sey 2 (SIMFONI, Davies et al., 2007) Circumnuclear disc are at most marginally
stable to grav. inst. (Sloshman & Begelman, 1989; Collin & Zahn, 2008)
Discs around AGNs are ALSO stellar
NGC 1097 (Davies et al., 2007): HI disc less massive than stellar M
bh = 1.25x108 M
sun
1'' = 330 pc
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AGN10 - University Rome 3, September 13, 2012
Enhanced SF within circumnuclear discs
NGC 7469
1'' = 80 pc
HCN gas around AGNs' nuclei (Hsieh et al., 2008; Kohno et al., 2008) Scales larger than Davies et al.: ~ 500 pc Line ratios:
RHCN/CO = 0.39
RHCN/HCO+ = 1.9 enhanced SF?
Excess gas around the circumnucl. region accreting gas, in excessof hydr. equil. (Hsieh et al. 2008) This gas can only be accounted
for if it is accreting from a larger region
Evidence for backflowing gas within the cocoon
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AGN10 - University Rome 3, September 13, 2012
A possible explanation of the Lbol/LEdd – age connection
Davies et al. (2007): older starburst are associated with brighter AGNs
Model: high Pj higher p
bck
faster suppression of SF in the disc
AND higher Tdisc
higher Lbol
Detailed modelling of gas+stellar discs with external backflow