But the fix was a 1/4 inch by 1 inch strip of 1/4 inch foam self adhesive weather striping stuck on the edge of the memory stick so when I put the cover on, it would push the stick down in the slot. Not sure why the latches are not keeping it down all the way. I looked close and could see when I pressed on it, I was not flexing the stick but the stick was not seated in the slot fully. But when I removed my finger the computer crashed.

It booted right up and said I had changed the amount of memory. I had nothing to lose, so I set the laptop on its side, gently pressed on the second (top) memory stick and hit the power button. Looking around the net for options I ran across a fix for Toshiba where the slot just needed a little pressure so the stick made good contact with the slot. Pulled stick one and put stick two in it booted right up. I had a 4G stick in slot one and went to put a matching stick in slot two. Stripped gas in the wake is mixed efficiently with intracluster gas already a few tens of kpc behind the disk, and this gas is free of residual star formation.I know this is a bit late for you but someone may find this info useful going forward. On the other hand, galaxies experiencing only mild ram pressure actually show an enhanced star formation rate that is consistent with observations. Depending on the inclination angle, this can light up a galaxy for a few hundred Myrs until all of the gas is stripped or consumed and star formation drops to almost zero, suggesting a typical quenching timescale of ~200 Myr. The cold gas disk is only stripped completely in extreme cases, leading to full quenching and significant reddening on a very short timescale. Star formation in our model galaxies is quenched mainly because the hot gas halo is stripped, depriving the galaxy of its gas supply.

As long as the disk is not completely stripped in peaks of RPS during pericentre passage, some gas that remains bound to the galaxies is redistributed to the outer parts of disks as soon as the ram pressure becomes weaker again, an effect that is not captured in simplified treatements of RPS. In most cases, the actual stripping radius of the simulated disk galaxies is larger than assumed in the SAMs, corresponding to an over prediction of the mass loss in SAMs. Results: We find that the stripping models employed in current SAMs often differ substantially from our direct simulations. Stellar light maps and the evolution of galaxy colours are computed with the stellar synthesis code FSPS to draw conclusions about quenching timescales of our model galaxies. Cooling, star formation, and stellar feedback are included according to a simple sub-resolution model. We use the moving-mesh code AREPO, augmented with a special refinement strategy to yield high resolution around the galaxy on its way through the cluster in a computationally efficient way. Methods: Our set-up employs a live model of a galaxy cluster that interacts with infalling disk galaxies on different orbits. We also analyse the gaseous wake of the galaxy, focusing on gas mixing and metal enrichment of the intracluster medium (ICM). In particular, we compare our findings for the mass loss and evolution of the star formation rate in our simulations with prescriptions commonly employed in SAMs. P ram u i u j the speed of the galaxy relative to the medium. This pressure can strip gas out of the galaxy where, essentially, the gas is gravitationally bound to the galaxy less strongly than the force from the intracluster medium wind due to the ram pressure. The exact cause of the environmental dependence is still poorly understood, yet semi-analytic models (SAMs) of galaxy formation need to parameterise it to reproduce observations of galaxy properties.Īims: In this work, we use hydrodynamical simulations to investigate the quenching of disk galaxies through ram-pressure stripping (RPS) as they fall into galaxy clusters with the goal of characterising the importance of this effect for the reddening of disk galaxies. Evidence of this ram pressure stripping can be seen in the image of NGC 4402. Observationally, the quenching of star-forming galaxies appears to depend both on their mass and environment.

Ram pressure striping