scholarly journals Systematics of Dwarf Novae

1987 ◽  
Vol 93 ◽  
pp. 3-13
Author(s):  
B. Warner

AbstractFrom about 30 Dwarf Novae with the best determined distances the following relationships are found.(i)a tight correlation between absolute magnitude at maximum light, Mv (max), and orbital period, P.(ii)a correlation between Mv (min) and P showing wide scatter.(iii)a correlation between Mv (mean), the mean absolute magnitude averaged over normal outbursts, and P, again with wide scatter. The scatter is shown to correlate strongly with outburst timescale Tn.(iv)a strong correlation between range, Mv (min) - Mv (max), and Tn (the Kukarkin-Parenago relationship).(v)a strong correlation between range My. (mean) - Mv (max), and both Tn and P.This final correlation is interpreted in terms of the disc instability model of dwarf novae and successfully predicts the observed width of outburst versus P relationship.

1979 ◽  
Vol 46 ◽  
pp. 89-95
Author(s):  
Frank M. Bateson

Abstract.The mean cycles and types of maxima for a number of dwarf novae are tabulated. It is shown that supermaxima are not confined to dwarf novae of short mean cycles. The decline rates for some stars are examined to ascertain if the orbital period, accurate to within ten percent, could be derived from visual observations. It is shown that, at least for some stars, the rate of decline differs widely at different levels of brightness, and, also, between dissimilar maxima of the same star.


Author(s):  
Nalan Hakime Nogay

AbstractBackground:Most of the studies investigating the correlation between the atherogenic index of plasma (AIP) and cardiometabolic risk factors have been conducted with adults, while only a limited number of related studies that involved children and adolescents has been conducted. The purpose of this study is to assess the correlation between the AIP and other cardiometabolic risk factors in adolescents.Methods:This study was conducted with 310 girls and 90 boys who were between the ages of 6 and 18 years. After a 10-h fasting period, the biochemical values of the participants were measured in the morning. The anthropometric measurements of the participants were also taken. The AIP was calculated as Log10 (triglycerides/high density lipoprotein-cholesterol; TG/HDL-C).Results:In adolescents between the ages of 12 and 18, the mean AIP of the group with TG ≥130 mg/dL was significantly higher than that of the groups with TG of 90–129 mg/dL and <90 mg/dL. There was a strong correlation between TG and AIP for both boys and girls among the children and adolescents, while there was a strong correlation between the TG/HDL-C ratio and TG only in the boys who were within the 6–11-year-old age group.Conclusions:An increase in AIP is associated with cardiovascular risk factors in children and adolescents other than those seen in adults. Based on the TG/HDL-C ratio, the AIP may be superior as a complementary index in the assessment of cardiometabolic risks in children and adolescents.


1995 ◽  
Vol 10 ◽  
pp. 399-402
Author(s):  
A.E. Gómez ◽  
C. Turon

The Hertzprung-Russel (HR) diagram luminosity calibration relies basically on three kinds of data: trigonometric parallaxes, kinematical data (proper motions and radial velocities) and cluster distances obtained by the zero-age main sequence fitting procedure. The most fundamental method to calculate the absolute magnitude is the use of trigonometric parallaxes, but up to now, accurate data only exist for stars contained in a small volume around the sun. Individual absolute magnitudes are obtained using trigonometric parallaxes or photometric and spectroscopic calibrations. In these calibrations the accuracy on the absolute magnitude determination ranges from ±0.m2 in the main sequence to ±0m5 in the giant branch. On the other hand, trigonometric parallaxes, kinematical data or cluster distances have been used to make statistical calibrations of the absolute magnitude. The standard error on the mean absolute magnitude calibrations ranges from ±0m3 to ±0m6 on the mean sequence, from ±0m5 to ±0m7 on thegiant branch and is of about 1mfor supergiants.Future improvements in the absolute magnitude determination will depend on the improvement of the basic data from the ground and space. A brief overview of the new available data is presented. In particular, the analysis of the first 30 months data of the Hipparcos mission (H30) (from the 37 months data of the whole mission) allows to perform a statistical evaluation of the improvements expected in the luminosity determination.


1987 ◽  
Vol 93 ◽  
pp. 205-205 ◽  
Author(s):  
F. Verbunt

AbstractThe preliminary results of the analysis of more than 1000 spectra of cataclysmic variables in the archive of the International Ultraviolet Explorer were presented at the meeting. To characterize the slope of the spectra I use F = log(f1460Å/f2880Å). For most spectra F lies between 0.2 and 0.7. No correlation of F with orbital period, inclination, system type or (for dwarf novae) length of the interoutburst interval are found, apart from somewhat lower values of F for DQ Her type systems. Out of 16 dwarf novae for which spectra both at outburst maximum and minimum are available 11 show no large difference in F between maximum and minimum, and in 5 F declines with the flux level. Out of 6 dwarf novae 5 show very red spectra during the rise to maximum, and 1 shows slopes during rise similar to those during decline.In the ultraviolet resonance lines, due to a wind from the disc, no correlation is found between inclination and terminal velocity.


2000 ◽  
Vol 175 ◽  
pp. 117-128 ◽  
Author(s):  
Danielle Briot ◽  
Noel Robichon

AbstractAbsolute magnitudes of Be and B stars are computed for each spectral type and luminosity class V and IV, using the Hipparcos parallax measurements. Some simulations have been carried out in order to estimate the effects which could bias the mean absolute magnitude calculations. As a result, only stars with σπ/π < 15% have been used. A first result is that B stars are fainter than previous estimations by about 0.5 magnitude on average. We then observe that on average Be stars are brighter than B stars of the same spectral type and this over-luminosity increases with the spectral type. A possible interpretation is proposed based on the fact that the rotational velocity of the late Be stars is near the critical rotational velocity.


2020 ◽  
pp. 120347542095763
Author(s):  
Hadas Zamir ◽  
Meora Feinmesser ◽  
Haim Gutman

Background/purpose This study examined clinical and histological parameters of primary dermal melanoma (PDM) to aid in its distinction from dermal metastasis. Methods Retrospective analysis of a prospective cohort of PDM patients. Includes patients fulfilling the strict histologic criteria for PDM ( N = 9) and patients who did not, but clinically, unequivocally had an intradermal melanoma—clinical PDM (cPDM; N = 17). Histopathology slides were re-examined. Prognosticators and outcome measures were compared between groups. Sentinel nodes’ retrieval and wide local excision (WLE) were offered to all patients as primary treatment. Results 26 patients identified, 15 females with a median age of 69 years (range 3.5-85). Mean Breslow was 7.9 ± 5.7 mm (median 5.8, range 1.8-25.0), and the mean mitotic rate was 4.9 ± 3.8/mm2 (median 4.0, range 0-17). Initial treatment and follow-up were as for cutaneous melanoma. One patient in each group with a palpable stage III underwent primary radical dissection. Sentinel nodes were retrieved in all 20 lymphatic mappings performed and found to be metastatic in 5 (25%) patients. Treatment consisted of completion lymph-node dissection. At a median postoperative follow-up of 62 months (range 8-132), 20 patients were disease-free, including 6 of 7 patients with stage III disease at presentation. Six patients died all of cPDM; 5 of 6 patients had primary ulcerated or epidermal-abutting melanomas. Conclusions This is the first study to highlight cPDM. Diagnosis requires expert pathology review and a tight correlation to the clinical parameters. Patients seem to benefit from WLE with sentinel node retrieval and complete dissection when appropriate. However, clinical guidelines for dissection have changed since the time period of this retrospective review. Based on this series, complete nodal dissection in these melanomas is associated with better than expected outcome, for stage III disease.


1979 ◽  
Vol 53 ◽  
pp. 494-494
Author(s):  
Karl W. Kamper

An Allegheny parallax series of SS Cyg, consisting of 52 exposures obtained on 15 nights, was recently measured on the PDS microphotometer at the David Dunlap Observatory, and a value of (m.e.) derived for the absolute parallax. This is close to the mean of the two previous discordant measures for this star given in the table below. The weighted mean of the three determinations implies that the absolute magnitude, at quiescent phase, of the star is between 7.0 and 9.0 formally at a 90% confidence level. Recent parallax determinations made at Lick by Vasilevskls et al. (1975) for three other stars, listed below along with the Mt. Wilson value for U Gem, imply even fainter absolute magnitudes.


1988 ◽  
Vol 108 ◽  
pp. 238-239
Author(s):  
Yoji Osaki ◽  
Masahito Hirose

SU UMa stars are one of subclasses of dwarf novae. Dwarf novae are semi-detached close binary systems in which a Roche-lobe filling red dwarf secondary loses matter and the white dwarf primary accretes it through the accretion disk. The main characteristics of SU UMa subclass is that they show two kinds of outbursts: normal outbursts and superoutbursts. In addition to the more frequent narrow outbursts of normal dwarf nova, SU UMa stars exhibit “superoutbursts”, in which stars reach about 1 magnitude brighter and stay longer than in normal outburst. Careful photometric studies during superoutburst have almost always revealed the “superhumps”: periodic humps in light curves with a period very close to the orbital period of the system. However, the most curious of all is that this superhump period is not exactly equal to the orbital period, but it is always longer by a few percent than the orbital period.


1986 ◽  
Vol 72 (5) ◽  
pp. 511-514 ◽  
Author(s):  
Cecilia Bozzetti ◽  
Nadia Naldi ◽  
Annamaria Guazzi ◽  
Rita Nizzoli ◽  
Magda Benecchi ◽  
...  

Estrogen receptor determination was performed on 120 breast cancer cytosols, using the dextran-coated charcoal method (DCC) and an enzyme immunoassay (EIA) to compare the efficiency of the two techniques. A strong correlation was noted between ER concentrations determined by DCC and EIA (P < 0.001). The mean ER-EIA value was significantly higher than the mean ER-DCC value in premenopausal (P < 0.001) as well in postmenopausal (P < 0.001) patients.


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