@article{SchmidtSaloSpahn2001,
  author    = {Schmidt, J{\"u}rgen and Salo, H. and Spahn, Frank},
  title     = {Viscous overstability in Saturn's B ring : II. Hydrodynamic theory and comparison to simulations},
  year      = {2001},
  language  = {en}
}
@article{SaloSchmidtSpahn2001,
  author    = {Salo, H. and Schmidt, J{\"u}rgen and Spahn, Frank},
  title     = {Viscous overstability in Saturn's B ring : I. Direct simulations and measurements of transport coefficients},
  year      = {2001},
  language  = {en}
}
@article{SaloPetzschmannSpahnetal.1999,
  author    = {Salo, H. and Petzschmann, Olaf and Spahn, Frank and Schmidt, J{\"u}rgen},
  title     = {Vertical distribution of temperature and density in a planetary ring},
  year      = {1999},
  language  = {en}
}
@article{ZaritskyCourtoisMunozMateosetal.2014,
  author    = {Zaritsky, Dennis and Courtois, Helene and Munoz-Mateos, Juan-Carlos and Sorce, Jenny and Erroz-Ferrer, S. and Comeron, S. and Gadotti, D. A. and Gil De Paz, A. and Hinz, J. L. and Laurikainen, E. and Kim, T. and Laine, J. and Menendez-Delmestre, K. and Mizusawa, T. and Regan, M. W. and Salo, H. and Seibert, M. and Sheth, K. and Athanassoula, E. and Bosma, A. and Cisternas, M. and Ho, Luis C. and Holwerda, B.},
  title     = {The baryonic Tully-Fisher relationship for S(4)G galaxies and the "condensed" baryon fraction of galaxies},
  series = {The astronomical journal},
  volume    = {147},
  journal   = {The astronomical journal},
  number    = {6},
  publisher = {IOP Publ. Ltd.},
  address   = {Bristol},
  issn      = {0004-6256},
  doi       = {10.1088/0004-6256/147/6/134},
  pages     = {11},
  year      = {2014},
  abstract  = {We combine data from the Spitzer Survey for Stellar Structure in Galaxies, a recently calibrated empirical stellar mass estimator from Eskew et al., and an extensive database of Hi spectral line profiles to examine the baryonic Tully-Fisher (BTF) relation. We find (1) that the BTF has lower scatter than the classic Tully-Fisher (TF) relation and is better described as a linear relationship, confirming similar previous results, (2) that the inclusion of a radial scale in the BTF decreases the scatter but only modestly, as seen previously for the TF relation, and (3) that the slope of the BTF, which we find to be 3.5 +/- 0.2 (Delta log M-baryon/Delta log v(c)), implies that on average a nearly constant fraction (similar to 0.4) of all baryons expected to be in a halo are "condensed" onto the central region of rotationally supported galaxies. The condensed baryon fraction, M-baryon/M-total, is, to our measurement precision, nearly independent of galaxy circular velocity (our sample spans circular velocities, vc, between 60 and 250 km s(-1), but is extended to v(c) similar to 10 km s(-1) using data from the literature). The observed galaxy-to-galaxy scatter in this fraction is generally <= a factor of 2 despite fairly liberal selection criteria. These results imply that cooling and heating processes, such as cold versus hot accretion, mass loss due to stellar winds, and active galactic nucleus driven feedback, to the degree that they affect the global galactic properties involved in the BTF, are independent of halo mass for galaxies with 10 < v(c) < 250 km s(-1) and typically introduce no more than a factor of two range in the resulting M-baryon/M-total. Recent simulations by Aumer et al. of a small sample of disk galaxies are in excellent agreement with our data, suggesting that current simulations are capable of reproducing the global properties of individual disk galaxies. More detailed comparison to models using the BTF holds great promise, but awaits improved determinations of the stellar masses.},
  language  = {en}
}
@article{SeissSpahnSremcevicetal.2005,
  author    = {Seiss, Martin and Spahn, Frank and Sremcevic, Miodrag and Salo, H.},
  title     = {Structures induced by small moonlets in Saturn's rings : implications for the Cassini Mission},
  issn      = {0094-8276},
  year      = {2005},
  abstract  = {Particle simulations are carried out to study density features caused by small moonlets embedded in a dense planetary ring. The creation of a "propeller" like structure is found together with adjacent density wakes. Both features are clear indications for the existence of moonlets in the rings. We confirmed that the propeller scales with the Hill-radius in radial direction whereas its azimuthal extent is determined by the ratio between the moonlet-mass and the ring-viscosity. Our findings bear direct implications for the analysis of the Cassini imaging (ISS) and occultation (UVIS) data: (i) for the detection of embedded larger bodies (>30 m) in Saturn's rings, and (ii) for remotely probing transport properties of the rings. The existence of a moonlet population may point to a catastrophic disruption of a parent body as a formation scenario for rings},
  language  = {en}
}
@article{SpahnSchmidtPetzschmannetal.2000,
  author    = {Spahn, Frank and Schmidt, J{\"u}rgen and Petzschmann, Olaf and Salo, H.},
  title     = {Stability analysis of a Keplarian disk of granular grains : influence of thermal diffusion},
  year      = {2000},
  language  = {en}
}