activity
20052015
most citedFrom dust to planetesimals: an improved model for collisional growth in protoplanetary disks

131 citations · 710 across the 17 of their papers we have counts for

collaborators

18 papers

astro-ph.GA2015★ 13 cited

GalevNB: a conversion from N-BODY simulations to observations

Xiaoying Pang, Christoph Olczak, Difeng Guo +2

We present (Galev for -body simulations), an utility that converts fundamental stellar properties of -body simulations into observational properties using the $GALE…

astro-ph.GA2015

GalevNB: Galev for N-Body simulations

Xiaoying Pang, Christoph Olczak, Rainer Spurzem

We report on GalevNB (Galev for N-Body simulations), an integrated software solution that provides N-body users direct access to the software package GALEV (GALaxy EVolutionary syn…

astro-ph.GA2015★ 66 cited

On the occurrence of galaxy harassment

Daniel Bialas, Thorsten Lisker, Christoph Olczak +2

Tidal interactions of galaxies in galaxy clusters have been proposed as one potential explanation of the morphology-density relation at low masses. The efficiency of tidal transfor…

astro-ph.SR2015★ 30 cited

Circumstellar discs in Galactic centre clusters: Disc-bearing B-type stars in the Quintuplet and Arches clusters

Andrea Stolte, Benjamin Hussmann, Christoph Olczak +7

We investigate the circumstellar disc fraction as determined from L-band excess observations of the young, massive Arches and Quintuplet clusters residing in the central molecular…

astro-ph.EP2013

Large grains can grow in circumstellar discs

Farzana Meru, Marina Galvagni, Christoph Olczak +1

We perform coagulation & fragmentation simulations to understand grain growth in T Tauri & brown dwarf discs. We present a physically-motivated approach using a probability distrib…

astro-ph.EP2013★ 35 cited

Growth of grains in Brown Dwarf disks

Farzana Meru, Marina Galvagni, Christoph Olczak

We perform coagulation and fragmentation simulations using the new physically-motivated model by Garaud et al. (2013) to determine growth locally in brown dwarf disks. We show that…