Superhumps: Comparison of observation, theory, and simulation

Smith, Amanda; Murray, J. R.; Haswell, C. A.; Truss, M. R.; Foulkes, Stephen B.

doi:10.1063/1.2816860

Cited by 2 publications

(2 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Mayer et al 2002) formation and in simulating astrophysical accretion discs(e.g. Smith et al 2007) and stellar collisions (e.g. Freitag & Benz 2005;Dale & Davies 2006) and publicly-available SPH codes such as GADGET-2 by Springel (2005) have found widespread application.…”

Section: Introductionmentioning

confidence: 99%

SPLASH: An Interactive Visualisation Tool for Smoothed Particle Hydrodynamics Simulations

Price¹

2007

Publ. – Astron. Soc. Aust

699

436

View full text Add to dashboard Cite

This paper presents splash, a publicly available interactive visualisation tool for Smoothed Particle Hydrodynamics (SPH) simulations. Visualisation of SPH data is more complicated than for grid-based codes because the data are defined on a set of irregular points and therefore requires a mapping procedure to a two dimensional pixel array. This means that, in practise, many authors simply produce particle plots which offer a rather crude representation of the simulation output. Here we describe the techniques and algorithms which are utilised in splash in order to provide the user with a fast, interactive and meaningful visualisation of one, two and three dimensional SPH results.

show abstract

Section: Introductionmentioning

confidence: 99%

SPLASH: An Interactive Visualisation Tool for Smoothed Particle Hydrodynamics Simulations

Price¹

2007

Publ. – Astron. Soc. Aust

699

436

View full text Add to dashboard Cite

show abstract

“…The period of the superhump (P sh ) is a few percent longer than those of the orbital period (P sh ). This slightly longer periodicity and the modulations are attributed to phase-dependent removal of the angular momentum in a tidally deformed eccentric disk (Whitehurst 1988;Hirose, Osaki 1990;Murray 1998;Smith et al 2007).…”

Section: Introductionmentioning

confidence: 94%

CCD Photometry of a Newly Confirmed SU UMa-Type Dwarf Nova, NSV 4838

Imada

Yasuda

Omodaká

et al. 2009

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

We present time-resolved CCD photometry of a dwarf nova NSV 4838 (UMa 8, SDSS J102320.27+440509.8) during the 2005 June and 2007 February outburst. Both light curves showed superhumps with a mean period of 0.0699(1) days for the 2005 outburst and 0.069824(83) days for the 2007 outburst, respectively. Using its known orbital period of 0.0678 days, we estimated the mass ratio of the system to be q=0.13 based on an empirical relation. Although the majority of SU UMa-type dwarf novae having similar superhump periods show negative period derivatives, we found that the superhump period increased atṖ /P sh =+7(+3, -4)×10 −5 during the 2007 superoutburst. We also investigated long-term light curves of NSV 4838, from which we derived 340 days as a supercycle of this system.

show abstract

Superhumps: Comparison of observation, theory, and simulation

Cited by 2 publications

References 1 publication

SPLASH: An Interactive Visualisation Tool for Smoothed Particle Hydrodynamics Simulations

SPLASH: An Interactive Visualisation Tool for Smoothed Particle Hydrodynamics Simulations

CCD Photometry of a Newly Confirmed SU UMa-Type Dwarf Nova, NSV 4838

Contact Info

Product

Resources

About