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Galactic Big Bang :MW Explosion

Yoshiaki SOFUE2013

銀河系の大爆発

Radio X Rays

Gamma Ray

BHS Model

AstronomicalExplosions

The Sun

Stars

Galaxies

The Universe

How about the MW?

Galactic Big Bang?

The North Polar Spur:

SNR 説Prof. Oort’ suggestion, 　　　 Spoelstra, 　　　　　 Berkhuijsen, 　　　 ROSAT PhD Thesis (SNR)….. et al.Even in Japan, 　　 Oda, Hayakawa, ...... et al　

Hayakawa et al. 1977Galactic Radio Loops I, II, III, IV

1.Galaxies1.GalaxiesStarburstStarburst 　 　

Shell / Outflow Shell / Outflow

M82

NGC 253ROSAT 0.75 keVPietsch et al 1999

NGC 253NGC 253 NGC 3079 NGC 3079 NGC 891NGC 891 NGC 4258 NGC 4258

NGC 30790.75 keV

2. Galactic Center

Gas, Mag. Fields, Cosmic rays outflows.

3x3 deg (400 x 400 pc) at 3 cm NRO 45m (Sofue, Handa et al.)

Cold gases are quiet: ring, clouds 2x0.5 deg (300 x 60 pc) (BTL 7m Bally et al.)

North Polar SpurNorth Polar Spur 408 MHz408 MHz

408MHz RadioHaslam et al 1982

408 MHz ROSAT 0.75 keV

2. Bipolar Hyper 2. Bipolar Hyper Shell Model for Shell Model for

NPSNPS

Sofue 1977

　 Fast MHD (compression) wave

Sofue 1977

Sofue 1977

Sofue 1977

EE 　　 ~~ 　　 101055-5655-56 ergs ergs 　　 ~~ 　　 10104-5 4-5 SNSN 　　 t t ~ 10~ 106-76-7 yr yr

Shock wavesShock waves E E ~ 1/2 ~ 1/2 MvMv22 　　 ~~ 　　 4π/3 ρ4π/3 ρrr33vv22

ρρ ～～ 1010-3-3 H/cc H/cc (Halo)(Halo) rr 　　 ~~ 　　 5 kpc5 kpc, , MM 　　 ~~ 　　 101077MM◎◎

vv 　　 ~~ 　　 200-300 km/s200-300 km/s Ｔ～ Ｔ～ 101077 K K→ → Soft X raysSoft X rays

Radial-rayadiabatic Shock Sakashita, Moellenhoff method

Bipolar Hyper Shell ModelBipolar Hyper Shell ModelSofue 1977, 1984 cf Tomiska, Ikeuchi 1988, Suchkov et al 1994

Numerical Hydrodynamics:Sofue & Habe 2013 (in prepa)

3. Simulationofof

ObservationsObservations

Radio synchrotron

RRadio emissivityadio emissivityB-CR equipartitionB-CR equipartition

εε∝∝ B Bγγ∝∝ ρραα

HI Disk & Arms

RadioNo arm

RadioArms

Obs. 408 MHz Obs.

Radio

408MHz RadioHaslam et al 1982

X-rays 0.25, 0.75, 1.5 keV Soft X-rays

XX-ray emissivity-ray emissivity BrehmsungBrehmsung εε∝∝ρρ22TT0.50.5

TransferTransfer:: Absorption bAbsorption by metals y metals in in HI DiskHI Disk

dI/ds=ε-κIdI/ds=ε-κI κds=dτ=nκds=dτ=nHHds/Nds/NH,0 H,0

X-ray Absorption X-ray Absorption κκ atat 0.25, 0.75, 1.50.25, 0.75, 1.5 keV keV

0.75 keV:0.75 keV: TauTau=1=1 for for

NNH,0H,0=3x10=3x1021 21 H cmH cm-2 -2 =1 kpc x=1 kpc x 1 H c1 H cmm-3-3

Sofue 1994 ApJL

Snowden et al. 1993

1.5 keVNo arm

0.75 keVNo arm

0.75 keVNo armCylinder/Cone

Soft X

0.25 kev

1.5 kev

0.75 kev

Arms

Galactic Big Bang15 Myr ago,1056 ergs.

Galxies: NGC 253

4. Implications4. Implications

MW Big Bang15 Myr ago,1055-56 ergs.

Implication Implication

Probing StarburstProbing Starburst Probing HI diskProbing HI disk Probing Gas HaloProbing Gas Halo Probing Halo-IGProbing Halo-IG Interface Interface Probing IProbing ICM, IGMCM, IGM PProbing Halo Windowrobing Halo Window

HI(red)+H2(green)HI(red)+H2(green)Nakanishi & SofueNakanishi & Sofue20062006

Galactic big bang in an intergalactic wind

5. The End of 40 yrs Debate

vs SNR hypothesis!

Fermi Bubble

Fermi Gamma rays1, 2, 5, 10 GeV

MW big bang model: 15 Myr ago, 1056 ergs.Sofue since 1970’

Radio X Rays

Gamma Ray

BHS Model

Radio+Gamma

X + Gamma

Gamma Ray

Further models to appear