Publications of the Astronomical Society of Australia

By A. Yonehara, Ryoji Takahashi. 2000

327 citations recorded by the source corpus.

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Citations in the corpus

A new class of accurate, mesh-free hydrodynamic simulation methods (2014, background): “This is a well-known result (Maddison et al. 1996; Imaeda & Inutsuka 2002; Cullen & Dehnen 2010), and occurs because of the physical viscous instability (Lyubarskij et al. 1994), except that the disk is supposed to be inviscid!”
Evolution towards the critical limit and the origin of Be stars (2007, result): “Keller (2004) measured the rotational velocity of 100 MS early B-type stars in clusters of the LMC and compared the results with observations of early B-type stars in clusters of the solar neighbourhood.”
A New Calibration Of Galactic Cepheid Period-Luminosity Relations From B To K Bands, And A Comparison To LMC Relations (2007, methodology): “…only eight Cepheids have been measured using the true IBW technique:δCep (Mérand et al. 2005), ηAql (Lane et al. 2002), βDor (Kervella et al. (2004c); Davis (2006)),ζGem (Lane et al. 2002), Y Oph (Mérand et al. 2007),ℓCar (Kervella et al. (2004b); Davis et al. (2006)), W Sgr (Kervella et al.…”
Science with the Murchison Widefield Array (2012, methodology): “Details on the technical design and specifications of the MWA are presented in a companion article (Tingay et al. 2012), which supercedes the earlier Lonsdale et al.”
The Baryon Content of Extremely Low Mass Dwarf Galaxies (2006, background): “For more luminous spiral galaxies, the average gas fraction is much lower: Bell & de Jong (2000) find an average gas fraction of 30% for a sample of low-inclination spiral galaxies.”
Microwave ISM Emission Observed by WMAP (2003, methodology): “Although warm ionized gas is well traced by Hα emission in three recent surveys (VTSS, Dennison et al. 1998; SHASSA, Gaustad et al. 2001; WHAM, Reynolds et al. 2003) as presented by Finkbeiner (2003) and corrected for dust using the Schlegel, Finkbeiner & Davis (SFD; 1998) dust map, one must worry…”
The 6-GHz multibeam maser survey-I. Techniques (2008, background): “Except for the first targeted survey by Menten (1991) and the survey of OH maser positions by Caswell et al. (1995) (with success rates exceeding 80 per cent, and further augmented by the discovery of offset and clustered maser sites), other targeted methanol maser searches have produced detection…”
The Evolution of the C/O Ratio in Metal-poor Halo Stars (2003, methodology): “Several previous works (e.g. Goswami & Prantzos 2000; Chiappini, Matteucci, & Romano 2001; Fenner & Gibson 2003; Prantzos 2003a) have successfully modelled the evolution of the Milky Way with two infall episodes (and no outflows); the first gives rise to the halo over a short time scale, while the…”
Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations (2009, background): “Building on pioneering work by Iben & Truran (1978) and Renzini & Voli (1981), various groups have published AGB yields (e.g. Forestini & Charbonnel 1997; van den Hoek & Groenewegen 1997; Marigo 2001; Chieffi et al. 2001; Karakas et al. 2002; Izzard et al. 2004).”
Gravitational Radiation from an Accreting Millisecond Pulsar with a Magnetically Confined Mountain (2005, background): “…the magnetic field into a narrow belt at the magnetic equator and increasing the field strength locally while reducing the global dipole moment (Melatos & Phinney 2000, 2001; Payne & Melatos 2004), in accord with observations of low- and high-mass X-ray binaries and binary radio pulsars (Taam…”
The 6-GHz methanol multibeam maser catalogue – II. Galactic longitudes 6° to 20° (2010, methodology): “A position was obtained in 2000 by Caswell (2009) with a peak flux density of only 3.5 Jy.”
A Full-Sky Hα Template for Microwave Foreground Prediction (2003, background): “The fast optics and low-noise CCD result in sub-rayleigh sensitivity at confusion limited levels (Dennison et al. 1998).”
Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, background): “The former quantity is a proxy of the mean stellar density ρ̄ (Ulrich 1986), while the latter has been shown to scale with the surface gravity and effective temperature (Brown et al. 1991; Kjeldsen & Bedding 1995; Bedding & Kjeldsen 2003)”
THE STRUCTURE OF CLASSICAL BULGES AND PSEUDOBULGES: THE LINK BETWEEN PSEUDOBULGES AND SÉRSIC INDEX (2008, background): “For a review of the properties of Sérsic profiles see Graham & Driver (2005).”