SUMMARY OF PROPOSAL 51031
KYOTO UNIV.
KYOTO JAPAN 606-01
KYOTO
KITASHIRAKAWA-OIWAKE-CHO, SAKYO
Tel: 075-753-3833 Fax: 075-701-5377
Medium: 2.5GB8MM
Subject: STARS
ROTATION PERIOD OF THE CENTRAL OBJECT OF BIPOLAR FLOW
ABSTRACT
With the PV phase observation of the Rho-Oph dark cloud, we found hard X-ray emission from class 1 sources. From these objects, we found bipolar flow with the radio observations. These put the sources to be protostars at dynamical mass accretion phase. One of the hard X-ray sources (EL29) shows a flare and other (WL6) shows sinusoidal variation suggesting star rotation of the protostar. Our proposal is to confirm this time variability (whether it is regular sinusoidal variation or not) and to make higher spatial resolution observation (observe at on axis position) to resolve source confusion and to search for X-rays from a younger object in the Rho-Oph cloud.
CO-INVESTIGATORS
| CO-I NAME | INSTITUTE | COUNTRY |
|---|
| SHIRO UENO | KYOTO UNIV. | JAPAN |
| YHOKO TSUBOI | KYOTO UNIV. | JAPAN |
| KENJI HAMAGUCHI | KYOTO UNIV. | JAPAN |
TARGETS
| TARGET NAME | PRI | RA | DEC | TIME | TC | OFF | GIS | SIS CNT | OBS |
|---|
| 1)RHO OPH CORE | 1 | 246.8392 | -24.4967 | 100 ks | N | Y | P | 0.20000 | 1 |