Dge, UK) (ESO) (Reipurth/HST/NASA) ESA Neii X-Raysshocks from Against ISM Young Stellar Objects Shock Temperature and Their Impact on the Stellar Environment

X -Ray Jets from Young Stars

Manuel Güdel University of Vienna HH34 HH111

Herbig-Haro Objects

100-400 km s-1 Outline

• Herbig-Haro Objects

• Inner Jets Manuel Güdel ETH• CoolingZürich Protostar Switzerland • Heating Manuel Güdel (University of Vienna),

Barbara Ercolano (Munich, Germany), • Conclusions James Owen (Cambridge, UK) (ESO) (Reipurth/HST/NASA) ESA NeII X-RaysShocks from against ISM Young Stellar Objects Shock temperature and their Impact on the Stellar Environment

(Raga et al. 2002) requires a few 100 km s-1: OK

Luminosity for radiative or non-radiative shock:

Manuel Güdel

ETH Zürich

Switzerland

(Raga et al. 2002) typically works OK (L ≈ 1029-31 erg s-1). Manuel Güdel (University Xof Vies Owen (Cambridge, UK) 6 29 -1 HH 2 (Orion): at bow shock of HH object, 10 K, LX ≈ 5x10 erg s

V = 200 km s-1 shock HST required for heating

measured motion: 230 km s-1

(Pravdo et al. 2001) 30 -1 HH210 (Orion): T = 0.8 MK in fastest HH feature, LX ≈ 10 erg s :

V = 170-240 km s-1 required shock observed bow-shock velocity 133-425 km s-1

X-rays

HST [SII]

(Grosso et al. 2006) HH 80/81 (from very luminous source)

6 31 -1 1.5x10 K, LX ≈ 4.5x10 erg s

-1 Vshock = 320 km s required

some optical features are much faster (600-1400 km s-1)

(Pravdo et al. 2004; contours: HST H) X opt (HST; NASA/ESA) X Cepheus A East & West: HH168

X 6.4x106 K, L ≈ 1.7x1030 erg s-1 H X

X-rays behind Hα:

cooling post-shock gas?

-1 Vshock = 280-680 km s sufficient

~consistent with optical line width in some places (200-600 km s-1)

(Pravdo et al. 2005, Schneider et al. 2009) [OI] (Dougados et al. 2000) DG Tau X-Rays (Güdel et al. 2005/08))

X-rays located close to jet base: Internal shocks, or collimation shocks?

5” L1551 IRS5, binary protostar (Favata et al. 2002, Bally et al. 2003) Jet Base?

L1551 IRS 5 Star absorbed, inner jet X-ray strong

• Cooling jet due to expansion • standing structure at 0.5-1”

(Schneider+ 2011)

3 spectra over 1 week Spectroscopic X-Ray Jets DG Tau soft/cool: hard/hot: variable hard/hotconstant

high NH low NH >> NH(AV)

? (Güdel et al. 2010)

Coronal (hard) emission absorbed by dust-depleted accretion flows with 22 -2 NH > 10 cm

Extreme case: edge-on Sz 102

Spectrum very soft, T = 2.1 MK star absorbed, see only jet?

ESA 0.3” Chandra ACIS-S image, soft band (0.3-1.5 keV)

T = 1.8-3.3 MK -1 vshock = 350-470 km s Deconvolution of SER-treated ACIS data (Güdel+ 2012) 1pixel = 0.0615”

0.15” (33 AU along jet)

2-8 keV

0.3-1.5 keV

T = 3.8 MK -1 vshock = 500 km s

Offset in 2010 approx. identical to 2005/06 (Schneider et al.: POSTER P47): standing structure; collimation region! Complete picture of DG Tau X-ray jet filling factor f Radiative Cooling

DG Tau: EM = 1.39x1052 cm-3 f = 3.5x10-5 43 -3 6 -3 V = 1.77x10 cm ne = 4.8x10 cm T = 3.7x106 K τ = 0.6 yr 29 -1 LX = 1.8x10 erg s

IRS 5: EM = 8.0x1051 cm-3 f = 1.23x10-5 45 -3 5 -3 V = 5x10 cm ne = 3.6x10 cm T = 7.0x106 K τ = 15 yr 28 -1 LX = 8.0x10 erg s DG Tau

0.35”

(Dougados et al. 2008) half opening angle for DG Tau ≈ 10 deg

(Agra-Amboage+ 2011: possibly smaller) Cooling of inner source including expansion initial radius: 0.1” half opening: 10 deg

DG Tau

6 -3 Requirement: Cooling time ~0.6 yrs: n0 > 10 cm L1551 IRS5

(Schneider et al. 2011) Pressure in the Plasma: Stationary Source

(Lavalley-Fouquet et al. 2000)

optical n ≈ 106 cm-3 T ≈ 104 K nT = 1010 K cm-3 DG Tau 6 -3 6 13 -3 X-ray ne = 4.8x10 cm T ≈ 3.7 x10 K nT = 1.8x10 K cm

(Itoh et al. 2000)

optical n ≈ 106 cm-3 T ≈ 104 K nT = 1010 K cm-3 IRS 5 5 -3 6 12 -3 X-ray ne = 3.6x10 cm T ≈ 7 x10 K nT = 2.5x10 K cm

Hot gas contributes to jet expansion if not located at surface of jet or confined by magnetic fields Origin of X-Ray Sources

X-ray shocks in collimation region

X-ray scattering

Colliding winds/jets from the two components

(Bally et al. 2003) Rhodos, 10 July 2008 NeII X-Rays fromShocks Young Stellar Objects and their Impact on the For high-T plasma close to star (L1551 IRS5, DG Tau) measured shock Stellar speeds 50 -100Environment km/s (Agra-Amboage et al. 2009, Lavalley-Fouquet et al. 2000)

Even bulk flow speeds often < 300 km s-1

But then, shock temperatures

Manuel Güdel ETH Zürich Switzerland (Raga et al. 2002) too low. Manuel Güdel (University of Vies Owen (Cambridge, UK) Plasma Mass Loss Rate A DG Tau: radiative heating dominates in center d radiative decay time

cooling distance

emission measure

(Agra-Amboage+ 2011)

Small amount of high-velocity gas that has escaped detection in the optical? (Günther et al. 2009) NeIIPulsed jetsX -Rays from X- rays density • Periodically ejected Young blobs Stellar Objects • Random velocity and their Impact on the Collisions between blobs Stellar Environment and environment: knots

Depending on shocks, chains of X-ray knots

especially in low-density jets

mostly at jet base Manuel Güdel ETH Zürich Higher ejection rate  Switzerland

higher LX Manuel Güdel (University of Vienna), Barbara Ercolano (Munich, Germany), James Owen (Cambridge, UK) (Bonito et al. 2010) density X-rays

density

Diamond shock at nozzle, 1500 km s-1  8 MK (Bonito et al. 2011 for L1551 IRS5) Reconnection

(Montmerle et al. 2000):

Winding up star-disk fields

 Antiparallel fields  Heating and Reconnection  Ejection of hot plasmoids  Further shock heating  Jets?

(Hayashi et al. 1996) Photoevaporation by X-Ray Jets?

Mass loss rate absorbed star from DG Tau disk jet dominated by jet irradiation at

r > 22 AU

X (Owen et al. in prep.)

…although this wind does not compete with accretion:

-10 -1 star: dM/dt ≈ 3x10 M yr -10 -1 jet: dM/dt ≈ 7x10 M yr HH OBJECTS: HH81 ç√HH168 -Cep A HH210 HH2

ç√

JETS: L1551 ç√ DG Tau IRS5 Z CMa HD 163296 OMC-3 RY Tau

“SPECTROSCOPIC X-RAY JETS”: DG Tau GV Tau DP Tau HN Tau Sz 102 Beehive NeII Conclusions

• X-rays found in protostellar and T Tauri jets from the base (collimation region?) to distant Herbig-Haro objects Manuel Güdel • Plasma close ETHto stars: Zürich high densities in standing structure Switzerland

Manuel • GüdelHeating: (University shocks or magnetic? of Vienna),

Barbara• ImportantErcolano influence (Munich, on protoplanetary Germany), disks: James heating, Owen ionisation, (Cambridge, chemistry, UK) photoevaporation NeII X-Rays from Young Stellar Objects and their Impact on the Stellar Environment END

Manuel Güdel ETH Zürich Switzerland

Manuel Güdel (University of Vienna), Barbara Ercolano (Munich, Germany), James Owen (Cambridge, UK) ESA