Binary

Binary seperation = 5 AU

Secondary mass= 0.15 SM

Secondary accrete gas around it

Isothermal temp = 1000 K

Primary's parameters:

Primary mass = 1 SM

Base density is fixed at 1.18E-5 g/cc throughout the primary (even in equatorial outflow)

Alpha of the secondary is 1. Alpha of the primary varies as below:

The velocity at the base of the wind does vary near the equatorial plane. In order to mimic the equatorial outflow induced by the in fall of planet (more massive than Jupiter), its open angle is (1/9)*Pi. Its velocity surges from 0.04 km/s to 2.4 km/s. Then equatorial outflow last only for 0.6 yr and start at frame= 150, i.e. time= 16.5 yr

Density plot + vector velocity of mid-plane:

density.gif​

Z-Angular momentum + density contour of mid-plane:

The whole angular momentum is negative, i.e. anti-clockwise. Which means, angular momentum has been transferred from stars to gas.

Lz.gif​

This simulation is basically based on Parker's model. The disk is not obvious and the pulsation is also not clear. The pulsation is subsonic and smeared out by the high density gas around the primary.

Which is supposed to be seen if the simulation is correct? Disk or spiral shock?

Attachments (5)

Comments

No comments.