Cien anos de soledad: The Novel as Myth and Archive

Echevarría, Roberto González

doi:10.2307/2906193

Cited by 21 publications

(9 citation statements)

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“…The data shown in Figs. 1 and 2 confirm many results obtained previously, and shows clustering of the objects, depending on their orbital periods, above the main sequence at minimum (Echevarria 1984;Echevarria, Costero & Michel 1993). This region is a very large one, reflecting differences in types of dwarf novae.…”

supporting

confidence: 85%

Simultaneous Multiwavelength Observations of Dwarf Novae Systems at Quiescence and in Outburst

Tovmassian

Echevarría

Pérez

et al. 1996

International Astronomical Union Colloquium

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The results of photometric and spectroscopic observations of dwarf novae are presented. The data were obtained during an international program of multiwavelength observations, held in 1986 February at several observatories, of dwarf novae during the first and subsequent days of outburst. During the campaign numerous dwarf novae were monitored in order to catch them in outburst. Preliminary results and analysis of some objects are reported elsewhere. A total of 30 dwarf novae were observed in the northern and southern hemispheres. Among them 37% were caught in outburst, including 10% on the rise to outburst and 17% in decline. Photometric observations were carried out in the UBVRI system and colour indexes were calculated.

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supporting

confidence: 85%

Simultaneous Multiwavelength Observations of Dwarf Novae Systems at Quiescence and in Outburst

Tovmassian

Echevarría

Pérez

et al. 1996

International Astronomical Union Colloquium

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“…A check for the I-band, which is at an effective wavelength ),8000 for an M5.5 dwarf (Bessell 1986), gives an absolute magnitude in I KC of 9.47 (+0.50/-0.70), giving an R -I of 1.22 (+0.16/-0.15). This is even redder than the R -I of 0.97 of U Gem (Echevarria 1984).…”

Section: Spectrum and Red Starmentioning

confidence: 70%

The Cataclysmic Variables from the Palomar-Green Survey

Ringwald¹

1993

PASP

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This thesis explores the cataclysmic variables (CVs) found by the Palomar-Green (PG) survey. This is the first compilation of a statistically complete sample of CV s found by ultraviolet color excess, and not outburst behavior. Blue and red follow-up spectrophotometry suggests that 22 of 68 objects classified originally as CV s are hot subdwarfs.Cool companions may be mimicking CVs' flat energy distributions, although the possibility remains that some are face-on CV s. Spectra taken with the International Ultraviolet Explorer satellite prove useful for distinguishing difficult cases.With the CV sample defined, the orbital periods for eleven systems are investigated with radial velocity studies. At 16th magnitude, CV number counts increase by 2.3 mag-I, although this may level off. The luminosity function is examined for the first time, and a trend toward higher space density at low luminosity is suspected. Outburst properties are compiled, and low-luminosity dwarf nove inflate the total space density to 6 x 10-6 pc-3 . I I describe all the PG CV s and candidate objects, and show spectra for most. This sample should be useful for population studies, such as measuring the space density with trigonometric parallaxes, or finding the fraction of eclipsing CV s.A new class of nova-likes, the SW Sextans stars, is characterized by absorption events of the emission lines at spectroscopic phase 0.5, accompanied by large phase lags between the lightcurves and the radial velocity curves and strong high-excitation emission.There are at least six such CVs in this sample of 33, so this mysterious behavior must be common and not peculiar, as previously thought. Five of these six objects eclipse._Serendipitous results for individual CVs include finding low-frequency quasi-periodic variations in the radial velocity curve of the dwarf nova BZ Ursa Majoris. While erratic from epoch to epoch, these are too coherent to be pure noise. Another dwarf nova, HX Pegasi, is caught with time-resolved spectrophotometry on the rise to outburst. This is the second-ever such observation, and the first with red spectra. HX Pegasi is also confirmed as having a novel subdwarf-K red star. II

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“…The colour indices reached the extreme values some 20 d later, around the time of the slope-break of the broken power-law decline, at T ≃ 54-58: B-V = 0.32 ± 0.05, V-R = 0.48 ± 0.03, R-I = 0.55 ± 0.03. These colours are redder than in most dwarf novae in quiescence (Echevarria 1984;Echevarria & Jones 1984;. The colours then turned back to becoming bluer.…”

Section: Long-term Light Curve and The Colour Evolutionmentioning

confidence: 96%

The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7−311525

Neustroev

Marsh

Zharikov

et al. 2017

Mon. Not. R. Astron. Soc.

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We report extensive 3-yr multiwavelength observations of the WZ Sge-type dwarf nova SSS J122221.7−311525 during its unusual double superoutburst, the following decline and in quiescence. The second segment of the superoutburst had a long duration of 33 d and a very gentle decline with a rate of 0.02 mag d −1 , and it displayed an extended post-outburst decline lasting at least 500 d. Simultaneously with the start of the rapid fading from the superoutburst plateau, the system showed the appearance of a strong near-infrared excess resulting in very red colours, which reached extreme values (B − I ≃ 1.4) about 20 d later. The colours then became bluer again, but it took at least 250 d to acquire a stable level. Superhumps were clearly visible in the light curve from our very first time-resolved observations until at least 420 d after the rapid fading from the superoutburst. The spectroscopic and photometric data revealed an orbital period of 109.80 min and a fractional superhump period excess 0.8 per cent, indicating a very low mass ratio q 0.045. With such a small mass ratio the donor mass should be below the hydrogen-burning minimum mass limit. The observed infrared flux in quiescence is indeed much lower than is expected from a cataclysmic variable with a nearmain-sequence donor star. This strongly suggests a brown-dwarf-like nature for the donor and that SSS J122221.7−311525 has already evolved away from the period minimum towards longer periods, with the donor now extremely dim.

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Cien anos de soledad: The Novel as Myth and Archive

Cited by 21 publications

References 0 publications

Simultaneous Multiwavelength Observations of Dwarf Novae Systems at Quiescence and in Outburst

Simultaneous Multiwavelength Observations of Dwarf Novae Systems at Quiescence and in Outburst

The Cataclysmic Variables from the Palomar-Green Survey

The remarkable outburst of the highly-evolved post period-minimum dwarf nova SSS J122221.7−311525

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