high energy activity on young stellar objects - activity of the x-ray lab. in 2005 -

High Energy High Energy Activity on Activity on

Young Stellar Young Stellar ObjectsObjects

- Activity of the X-ray Lab. - Activity of the X-ray Lab.

in 2005 -in 2005 -

Kenji Hamaguchi, Rob PetreKenji Hamaguchi, Rob Petre

Activity of the X-ray Lab.Activity of the X-ray Lab.

• Study of the X-ray activity on YSOs– Intermediate-mass eclipsing binary, TY CrA– X-ray monitoring of an FU/EX Ori outburst– X-ray activity on Herbig Ae/Be stars

• New observations– Suzaku: 73P/Schwassmann-Wachmann 3– XMM-Newton: a young eclipsing binary– Chandra & HST: HAes (collaboration w/C. Grady)– More Chandra proposal on this cycle (w/Carol)

Outburst of V1647 Ori

Strong correlation between optical/IR and X-raysX-ray emission is originated in mass accretion

Activity of the X-ray Lab.Activity of the X-ray Lab.

• Study of the X-ray activity on YSOs– Intermediate-mass eclipsing binary, TY CrA– X-ray monitoring of an FU/EX Ori outburst– X-ray activity on Herbig Ae/Be stars

• New observations– Suzaku: 73P/Schwassmann-Wachmann 3– XMM-Newton: a young eclipsing binary– Chandra & HST: HAes (collaboration w/C. Grady)– More Chandra proposal on this cycle (w/Carol)

Setbacks of Our Projects Setbacks of Our Projects

• ADP proposal for the archival research of the XMM data of star forming regions– ADP proposal was canceled last year.

• Suzaku observations– The launch was delayed (July 2005).

• It could not observe Tempel 9 at the Deep Impact.

– The XRS detector malfunctioned before actual observations.

Loss of XRS on SuzakuLoss of XRS on Suzaku• XRS (X-ray calorimeter)

– had the best energy resolution (E/dE ~1000)– malfunctioned before observations

• Suzaku has two types of detectors working– XIS (X-ray CCD) and HXD

• The spatial resolution is limited.• XIS BI chip has the best energy resolution so far

below 1 keV for diffuse sources.

Activity of the X-ray Lab.Activity of the X-ray Lab.

• Study of the X-ray activity on YSOs– Intermediate-mass eclipsing binary, TY CrA– X-ray monitoring of an FU/EX Ori outburst– X-ray activity on Herbig Ae/Be stars

• New observations– Suzaku: 73P/Schwassmann-Wachmann 3– XMM-Newton: a young eclipsing binary– Chandra & HST: HAes (collaboration w/C. Grady)– More Chandra proposal on this cycle (w/Carol)

New Data Have Just Arrived!New Data Have Just Arrived!HD100453 (Chandra) EK Cep (XMM-Newton)

Activity of the X-ray Lab.Activity of the X-ray Lab.

• Study of the X-ray activity on YSOs– Intermediate-mass eclipsing binary, TY CrA– X-ray monitoring of an FU/EX Ori outburst– X-ray activity on Herbig Ae/Be stars

• New observations– Suzaku: 73P/Schwassmann-Wachmann 3– XMM-Newton: a young eclipsing binary– Chandra & HST: HAes (collaboration w/C. Grady)– More Chandra proposal on this cycle (w/Carol)

R C

rA s

tar

form

ing r

egio

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XM

M-N

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ton

, 20

03

Marc

h 2

8

Red: 0.2-1 keV

Green: 1-2 keV

Blue: 2-9 keV10’

TY CrA TY CrA - the only eclipsing - the only eclipsing Herbig Be binary system Herbig Be binary system

confirmed -confirmed -

Orbital Period, 2.88878 days

PrimaryB7-93.16Msolar

Secondary1.64Msolar

Tertiary1.2~1.4Msolar

0.065 AU

1-1.5 AU

Fourth~M4

0.3” (~40 AU)

X-ray observations(ASCA: 1994-98)• kT ~ 1.5 keV• Lx ~ 3e30 ergs s-1

Age ~3 Myr

TY CrA TY CrA - the only eclipsing - the only eclipsing Herbig Be binary system Herbig Be binary system

confirmed -confirmed -

Orbital Period, 2.88878 days

Primary eclipseMarch 28, 2003, 37ksec

Secondary eclipseMarch 29, 200333ksec

XMM-NewtonLarge effective area Best for observing time variation

Sim

ula

tions

of

X-r

ay lig

ht

curv

es

duri

ng t

he e

clip

se

Secondary Eclipse

Primary Eclipse

X-ray Spectrum in the Primary Eclipse

Primary eclipsekThot ~4 keVLog Lx ~ 2e31 (ergs s-1)

Secondary eclipsekThot ~1.5 keVLog Lx ~ 6e30 (ergs s-1)

Light Curve, Apr 2001

0.490.4 Orbital Phase

Secondary eclipsekThot ~4.5 keVLog Lx ~ 3e31 (ergs s-1)

Summary of the Summary of the ObservationsObservations

Low State (XMM 2nd obs. & ASCA obs.)Low State (XMM 2nd obs. & ASCA obs.) kTkThothot~1.5 keV, Lx ~3-6x10~1.5 keV, Lx ~3-6x103030 ergs s ergs s-1-1

No variation specific at optical eclipsesNo variation specific at optical eclipses Normal activity of some stars in the TY CrA Normal activity of some stars in the TY CrA

system?system? High StateHigh State

kTkThothot~4 keV, Lx ~2-3x10~4 keV, Lx ~2-3x103131ergs sergs s-1-1

X-ray flux increased at coincident with X-ray flux increased at coincident with eclipsing phases (of both the primary and eclipsing phases (of both the primary and secondary)secondary)

Enhanced inter-binary magnetic activity? The Enhanced inter-binary magnetic activity? The X-ray beaming effect?X-ray beaming effect?

X-ray Observations of TY X-ray Observations of TY CrACrA

Date Satellite kThot Log Lx State

(keV) (ergs s-1)

94/04/04 ASCA 1.8 30.4 LS

96/10/18 ASCA 1.8 30.5 LS

98/10/19 ASCA 1.2 30.6 LS

00/10/07 Chandra 2.0 (3.5) 30.7 (31.1) LS (+ Flare)

01/04/09 XMM 4.5 31.4 HS

03/03/28 XMM 3.9 31.2 HS

03/03/29 XMM 1.5 30.8 LS

Diagram of the HAe X-ray Activity

The high state originates from a temporal activity