Papers about stellar collisions with SPH

The SPH method was invented in 1977 independently by Gingold & Monaghan and Lucy to study the fission of rotating (proto)stars. In 1979, it was applied to investigate the disruption of a star due to the tidal pull of a companion (Gingold & Monaghan 1979). SPH simulations of collisions between interstellar gas clouds were done in 1985 by Lattanzio et al. and, in 1986 Benz et al. considered the collision between the proto-earth and a large object to explain the origin of the moon. The first published SPH simulations of stellar collisions are the ones by Benz & Hills (1987). The field has since grown to a small industry and keeping track of all publications is difficult. Here is an incomplete list, organized by collision type. In this table q stands for the mass ratio M_2/M_1; other quantities are defined here.

Collision type and regime
Lin et al 1998 (collisions between proto-stellar disks)
Zinnecker & Bate 2002 (conference proceeding discussing collisions between pre-MS stars in a young cluster; show how a low-mass star can be tidally disrupted by a more massive star)
Laycock & Sills 2005 (collisions between a pre-MS star and a variety of other stars)
Davies et al, 2006 (collisions involving pre-MS stars; discussion of how they may contribute to massive-star formation in young clusters)
MS -- MS low velocity
Lombardi, Rasio & Shapiro 1995,1996 (blue straggler formation; q=0.2-1)
Sandquist, Bolte & Hernquist 1997 (Study of the mixing during merger and blue straggler evolution)
Sills et al. 1997,2001 (SPH simuls to investigate structure and evol. of blue stragglers; up to Np=1e5)
Barnes 2000 (comparison with collision of galaxies; polytropes n=1.5; q=0.5/1)
Lombardi et al. 2002 (SPH simuls to validate semi-analytical model)
Sills et al. 2002 (up to Np=1e6 to determine blue straggler structure)
Lombardi et al. 2003 (Triple collisions, SPH simuls used to demonstrate applicability of fluid sorting method)
Sills, Adams & Davies 2005 (Concentrate on effect of rotation on structure and evolution of blue straggler)
Dale & Davies 2006 (Collisions involving massive stars; discuss evolution of collision product in context of GRB and formation of very massive stars)
Suzuki et al. 2007 (Collisions involving massive stars and evolution of merger product in the context of "runaway" growth of very massive stars in clusters)
Trac, Sills & Pen 2007 (Comparison between SPH and grid code [TVD] for equal-mass, 0.8 Msun collisions)
Gaburov et al. 2007 (Collisions involving massive stars; extend and test fluid sorting algorithm for this regime)
MS -- MS high velocity
Benz & Hills 1987 (polytropes n=1.5; Np=1000; q=1; 0-2.33*V_star)
Benz & Hills 1992 (polytropes n=1.5; Np=7000; q=.2; 0-5*V_star)
Lai, Rasio & Shapiro 1993 (Eddington models, n=3; Np=8000; q=0.1-1; 0.2-3.8*V_star)
Rauch 1999 (simul. by M. Davies) (polytropes n=3; q=0.25-1; 1-25*V_star)
Freitag 2000 (Thesis) (realistic stars; Np=2000-36000; q=0.001-1; 0.1-30*V_star)
Freitag & Benz 2005 (basically the same but published ;-) )
MS -- more compact
Davies, Benz & Hills 1992 (Giant--NS and MS--NS)
Davies et al. 1993 (equal-mass MS--WD to compare SPH with grid method, Np up to 27000)
Lee, Kim & Kang 1996 (MS--NS, parabolic, d_min>R_MS, M_MS=0.2-0.7 M_sun)
Giant -- Giant

Giant -- more compact
Davies, Benz & Hills 1991 (0.8 M_sun Giant--0.4/0.6 M_sun point mass, parabolic; Np=7000)
Davies, Benz & Hills 1992 (Giant--NS and MS--NS)
Rasio & Shapiro 1991
Fryer & Woosley 1998, Zhang & Fryer 2001 (He star--BH merger in a binary as GRB engine)
Bailey & Davies 1999 (Giant--MS at Galactic center, M_giant=2-8 M_sun, V_rel up to 300 km/s)
Lombardi et al. 2006 (Subgiant/Giant--NS as a way to create Ultracompact X-ray binary)
WD -- WD
Benz, Hills & Thielemann 1989 (parabolic; 0.6--0.6 M_sun + 0.7--0.9 M_sun; Np=5000)
Benz et al. 1990 (merger in circular binary)
Segretain, Chabrier & Mochkovitch 1997 (mergger in circular binary)
WD -- more compact
Fryer et al. 1999 (WD--BH in a circularized binary as GRB engine)
NS -- NS (binary)
Rasio & Shapiro 1992,1994
Centrella & McMillan 1993 (q=1, parabolic; Np=2000/4000)
Davies et al. 1994
Rosswog et al. 1999
Faber & Rasio 2000,2002,Faber, Rasio & Justin 2001 (post-Newtonian)
Oechslin, Rosswog & Thielemann 2002 (Conform flat approx)
Rosswog & Davies 2002, Rosswog & Liebendörfer 2003, Rosswog, Ramirez-Ruiz & Davies 2003, (post-Newtonian; up to 1e6 particles)
NS -- BH (binary)
Lee & Kluzniak 1995, & Lee, Kluzniak & Wlodzimierz 1999a,1999b, Lee 2000,2001 (Newtonian gravity)
Wlodzimierz & Lee 2002 (Quark star-BH!)
Collisions featuring binaries
Cleary & Monaghan 1990 (binary -- single; n=1.5 polytropes with R~M-1/3; only ~180 part/star)
Goodman & Hernquist 1991 (binary -- binary; all MS)
Davies, Benz & Hills 1993,1994 (binary -- single, 3-body runs compared with SPH; binary: NS-MS intruder: NS/WD/MS)
Davies et al. 1998 (binary -- giant at Galactic center; 4-body checked with SPH runs)
Adams, Davies & Sills 2004 (binary -- giant in globular clusters)

A special category is the tidal disruption of a star by a massive black hole, at the center of a galactic nucleus.

See also the reference list for collision simulations with grid methods.