1931
DOI: 10.1056/nejm193107092050207
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Methods of Electrocardiography and the Normal Electrocardiogram

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Cited by 22 publications
(24 citation statements)
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“…There is a critical mass-transfer rate above and below which the system appears to be in two different states. This critical rate of mass loss from the main-sequence star iṡ M 2crit = −8.08 × 10 15 α H 0.3 0.3 (1 + q) 7/8 P h 7/4 g s −1 (48) (Faulkner et al 1983), where α H = 0.1. DNe lie below the critical value.…”
Section: Critical Mass-transfer Ratementioning
confidence: 94%
See 1 more Smart Citation
“…There is a critical mass-transfer rate above and below which the system appears to be in two different states. This critical rate of mass loss from the main-sequence star iṡ M 2crit = −8.08 × 10 15 α H 0.3 0.3 (1 + q) 7/8 P h 7/4 g s −1 (48) (Faulkner et al 1983), where α H = 0.1. DNe lie below the critical value.…”
Section: Critical Mass-transfer Ratementioning
confidence: 94%
“…The ratio of the atmosphere scaleheight to the radius of the star is comparable to the ratio of the mass lost from the system to its total mass, so the change in separation is not sufficient to shut off mass transfer altogether but does reduce the rate significantly. This change in rate could be responsible for the diversity of cataclysmic variable types at a given period: dwarf novae (DNe) that undergo disc instability outbursts require a lower mean mass-transfer rate than nova-likes (NLs) that do not suffer the disc instability (Faulkner, Lin & Papaloizou 1983). However the idea lost favour when it was realized that the nova ejecta would temporarily form a common envelope around the system and consequential angular momentum loss would actually cause lower-period systems to shrink (Livio, Govarie & Ritter 1991).…”
Section: Introductionmentioning
confidence: 99%
“…It is well known that models with constant values of a cannot reproduce the observed light curves of dwarf novae (Smak 1984b; see however Faulkner et al 1983). They predict that globally, the disc reaches neither the hot nor the cold branches.…”
Section: E Vo L U T I O N O F D Wa R F N Ova D I S C Smentioning
confidence: 99%
“…On the one hand, the disc instability model (e.g. Smak 1982;Faulkner, Lin & Papaloizou 1983;Ludwig et al 1994) predicts that the surface density values should lie between 10 and 100 g cm 22 for as between 0.1 and 1 and even larger Ss for smaller as. This means that the disc must have a massive, optically thick component.…”
Section: The Vertical Disc Structurementioning
confidence: 99%