The First Basic Problem Revisited: Reply to Commentaries on Howell Et Al. (2003)

Howell, Steve N. G.; Corben, Chris; Pyle, Peter; Rogers, Danny I.

doi:10.1650/7507

Cited by 8 publications

(5 citation statements)

References 13 publications

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“…Since this figure is only for a comparison purpose, we omit the table and source information for each SU UMa-type object to avoid too much complexity and simply list the objects as the form of a footnote. 6 In this diagram, ordinary SU UMa-type objects are widespread, while WZ Sge-type objects have surprisingly similar outburst "amplitudes" when superhumps start to appear. The mean and standard deviation of these values (excluding candidate period bouncers) are 6.4 and 0.7 mag, respectively.…”

Section: Absolute Magnitudes In Quiescencementioning

confidence: 91%

“…In recent years, the tendency is more striking after the increase of discovery by CRTS (Drake et al 2009), MASTER (Gorbovskoy et al 2013) and ASAS-SN (Shappee et al 2014;Davis et al 2015). In the most recent year of 2014, the contribution of the surveys are: CRTS (1), MASTER (1), ASAS-SN (9) and amateur discoveries (6). Although ASAS-SN has been discovering a great number of WZ Sge-type objects, widefield survey of bright transients by amateur astronomers still has a great impact in this field.…”

Section: Modern Criteriamentioning

confidence: 99%

“…Although we selected outbursts which were detected sufficiently close to the peak brightness, we should note that actual outbursts may have started slightly ear- On the right side, we show mass ratios estimated using equation (6). We can regard this figure as to represent an evolutionary diagram (see discussion in subsection 7.5).…”

Section: Delay Time Of Superhump Appearancementioning

confidence: 99%

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WZ Sge-type dwarf novae

Katô

2015

Publications of the Astronomical Society of Japan

161

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We have summarized the current understanding and recently obtained findings about WZ Sge-type dwarf novae. We also reviewed the historical development of the understanding of these objects, provided the modern criteria, and reviewed the past research in relation to superhumps, early superhumps and the outburst mechanism. We regard that the presence of early superhumps (reflecting the 2:1 resonance) and long or multiple rebrightenings are the best distinguishing properties of WZ Sge-type dwarf novae. We provided the updated list of nearly 100 WZ Sge-type dwarf novae mainly based on the data obtained by the VSNET Collaboration up to Kato et al. (2015) and discussed the statistics. We could detect early superhumps with amplitude larger than 0.02 mag in 63% of the studied WZ Sge-type dwarf novae, which makes early superhumps a useful distinguishing feature for WZ Sge-type dwarf novae. Theoretical light curves of early superhumps generally appear to reproduce the existence of many low-amplitude objects, supporting the geometrical origin of early superhumps. Using the recently developed method of measuring mass ratios using developing phase of superhumps (stage A superhumps), we showed that there is a linear relation between the period variation of superhumps and the mass ratio in WZ Sge-type objects. By using this relation, we were able to draw an evolutionary picture of a large number of WZ Sge-type and identified the type of outburst to be an evolutionary sequence: type C → D → A → B → E, with some outliers for type-B objects. The duration of stage A (evolutionary phase) of superhumps is also well correlated with the estimated mass ratios. By using mass ratios from stage A superhumps and durarion of stage A, we have been able to identify best candidates for period bouncers.

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Section: Absolute Magnitudes In Quiescencementioning

confidence: 91%

Section: Modern Criteriamentioning

confidence: 99%

Section: Delay Time Of Superhump Appearancementioning

confidence: 99%

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WZ Sge-type dwarf novae

Katô

2015

Publications of the Astronomical Society of Japan

161

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“…• The closest cataclysmic variable is WZ Sge at 43.5 pc Howell et al 2004). The intervals between its outbursts are, therefore, shorter than the light travel time, but not by an enormous factor, as it is one of the longestperiod dwarf novae.…”

Section: Extremamentioning

confidence: 98%

Astrophysics in 2004

Trimble

Aschwanden

2005

PUBL ASTRON SOC PAC

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“…Most recently, Howell (2010) seemingly hybridized the 2 approaches by defining molt strategy on the basis of number of insertions, which usually correspond to a particular inserted molt, within a given cycle. In response to critics, Howell et al (2004) reiterated that feather color should not be used to identify homologous molts and that molt homology should be considered ''comparable,'' awaiting verification of evolutionary origins when ''a genetic basis will eventually be discovered that can reveal homologies of molts'' (Howell et al 2004:207). Although H-P-H may be correct in assuming that an annual molt is highly conserved, note that timing of development is one of the most variable elements of evolution and that the vast majority of morphological evolution occurs through changes in developmental timing (West-Eberhard 2003).…”

Section: Molt Cyclementioning

confidence: 99%