Early Type Stars Observed with ASCA

• Classification– Wind Collision &

Single Star

• Objection on the Standard Line Driven Instabilities

• Elemental AbundanceSix Single Stars

Classification

• Colliding Wind Shock– HD19379 3.2 keV– γ2 Vel 0.3keV+1.4keV– V444 Cyg 0.6keV+2 keV– WR147 1keV dominant

• Single Stars– δOri 0.42 keV– CygOB２ 0.6~3.2 keV– τ　 Sco 0.49 keV +HT– λ　 Ori 0.35keV+ HT– ζ　 Ori 0.43 keV– ζ　 Oph0.54 keV– ζ　 Pup 0.59 keV V444 Cyg: Colliding Wind

Classification

• Others– 30 Dor

• BH Binaries?

– Planetary Nebula• Wind-flown Bubble?

– Eta Carinae • ?

ηCar 　ｂｙTsuboi et al. 1997Ｃｏｒｃｏｒａｎ et al. 1998

Objection to The StandardLine Driven Instability Model?

• Hot Component• τ 　Ｓｃｏ、 λ 　Ｏｒｉ

– Non Thermal Comp.

– Magnetic Origin?• Cohen et al. 1997

• Plan– Universal Analysis of all t

he ASCA data

Elemental Abundance

• Enrichment of Ne in HD193794

• Enrichment of N in ηCar– CNO Cycle processed

matter

• Metal Depletions in Early Type Stars

ηCar by Tsuboi et al.(1997)

Elemental Abundance

• Metal Depletions in Early Type Stars– Multiple Temp?

– Optically Thick?

– Real Depletion?

• Neuton’s Objective

Multi Temperature

Single Temperature

Proposal: Examination of the Standard Line Driven Instability

• Some Objections– Hard Tails in τ　 Sco

and λOri

– Evidence of Gas Ejection

Proposal: Examination of the Standard Line Driven Instability

• IUE Observation– Plasma fixed on the surface

of the star

– Possibly associated with large-scale magnetic structure

– Z-Pup

– HD64760

• X-ray Hard Tail– Magnetic Field?

Howarth et al. 1995

Proposal: Examination of the Standard Line Driven Instability

• Highly Variable in hard X-rays with a time scale of ~days

• Objective– Detection of Variability and study

of spectral change

• Plan– Z-Ori, 10ksec x 10 days

Z-Ori by ROSAT