arXiv subjects

L. L. Kiss

Publications and source records attributed to L. L. Kiss.

186 records · Page 11Linked to original sources

arXiv2000

Early spectroscopic observations of Nova (V1494) Aquilae 1999 No.2

Low- and medium resolution spectra of the fast nova, Nova (V1494) Aql 1999 No.2 obtained approximately 6, 7, 19 and 28 days after the maximum brightness are presented and discussed. The spectrum covering the whole optical range at day 6 shows the principal plus diffuse-enhanced spectrum. The presence of strong Fe II multiplets with P-Cyg profiles suggest that V1494 Aql belongs to the ``Fe II'' class defined by Williams (1992). The medium-resolution profiles (lambda/Delta lambda \approx 7000) of the Hgamma and Hdelta lines show well-defined sharp absorption features with the same radial velocities, while the Halpha split into two distinct emission peaks in the last two spectra (Delta t=19 and 28 days). The observed behaviour suggests an expanding equatorial ring with possible small-scale clumpiness in the nova shell. The visual lightcurve is used to deduce M_V by the maximum magnitude versus rate of decline relationship. The resulting parameters are: t_2=6.6+/-0.5 days, t_3=16+/-0.5 days, M_V=-8.8+/-0.2 mag. Adopting this value, a distance d=3.6+/-0.3 kpc is determined.

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arXiv1999

A photometric and spectroscopic study of the brightest northern Cepheids. III. A high-resolution view of Cepheid atmospheres

We present new high-resolution (R=40000) spectroscopic observations of 18 bright northern Cepheids carried out at David Dunlap Observatory, in 1997. The measurements mainly extend those of presented in Paper I adding three more stars (AW Per, SV Vul, T Mon). The spectra were obtained in the interval of 5900 A and 6660 A. New radial velocities determined with the cross-correlation technique and the bisector technique are presented. We found systematic differences between the spectroscopic and CORAVEL-type measurements as large as 1-3 km/s in certain phases. We performed Baade-Wesselink analysis for CK Cam discovered by the Hipparcos satellite. The resulting radius is 31+/-1 Ro, which is in very good agreement with recent period-radius relation by Gieren et al. (1999). Observational pieces of evidence of possible velocity gradient affecting the individual line profiles are studied. The FWHM of the metallic lines, similarly to the velocity differences, shows a very characteristic phase dependence, illustrating the effect of global compression in the atmosphere. The smallest line widths always occur around the maximal radius, while the largest FWHM is associated with the velocity reversal before the minimal radius. Three first overtone pulsators do not follow the general trend: the largest FWHM in SU Cas and SZ Tau occurs after the smallest radius, during the expansion, while in V1334 Cyg there are only barely visible FWHM-variations. The possibility of a bright yellow companion of V1334 Cyg is briefly discussed. The observed line profile asymmetries can be partly associated with the velocity gradient, which is also supported by the differences between individual line velocities of different excitation potentials.

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arXiv1999

CCD photometry and new models of 5 minor planets

We present new R filtered CCD observations of 5 faint and moderately faint asteroids carried out between October, 1998 and January, 1999. The achieved accuracy is between 0.01-0.03 mag, depending mainly on the target brightness. The obtained sinodic periods and amplitudes: 683 Lanzia - 4.6+/-0.2 h, 0.13 mag; 725 Amanda - >3.0 h, >=0.40 mag; 852 Wladilena - 4.62+/-0.01 h, 0.32 mag (December, 1998) and 0.27 mag (January, 1999); 1627 Ivar - 4.80+/-0.01, 0.77 mag (December, 1998) and 0.92 mag (January, 1999). The Near Earth Object 1998 PG unambiguously showed doubly-periodic lightcurve, suggesting the possibility of a relatively fast precession (P_1=1.3 h, P_2=5.3 h). Collecting all data from the literature, we determined new models for 3 minor planets. The resulting spin vectors and triaxial ellipsoids have been calculated by an amplitude-method. Sidereal periods and senses of rotation were calculated for two asteroids (683 and 1627) by a modified epoch-method. The results are: 683 - lambda_p=15/195+/-25 deg, beta_p=52+/-15 deg, a/b=1.15+/-0.05, b/c=1.05+/-0.05, P_sid=0.1964156+/-0.0000001 d, retrograde; 852 - lambda_p=30/210+/-20 deg, beta_p=30+/-10 deg, a/b=2.3+/-0.3, b/c=1.2+/-0.2; 1627 - lambda_p=145/325+/-8 deg, beta_p=34+/-6 deg, a/b=2.0+/-0.1, b/c=1.09+/-0.05, P_sid=0.1999154+/-0.0000003 d, retrograde. The obtained shape of 1627 is in good agreement with radar images by Ostro et al. (1990).

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arXiv1999

Multiperiodicity in semiregular variables - I. General properties

We present a detailed period analysis for 93 red semiregular variables by means of Fourier and wavelet analyses of long-term visual observations carried out by amateur astronomers. The results of this analysis yield insights into the mode structure of semiregular variables and help to clarify the relationship between them and Mira variables. After collecting all available data from various international databases (AFOEV, VSOLJ, HAA/VSS and AAVSO) we test the accuracy and reliability of data. We compare the averaged and noise-filtered visual light curves with simultaneous photoelectric V-measurements, the effect of the length versus the relatively low signal-to-noise ratio is illustrated by period analysis of artificial data, while binning effects are tested by comparing results of frequency analyses of the unbinned and averaged light curves. The distribution of periods and period ratios is examined through the use of the (log P_0, log P_1) and (log P_1, log P_0/P_1) plots. Three significant and two less obvious sequences are present which could be explained as the direct consequence of different pulsational modes. This hypothesis is supported by the results for multiperiodic variables with three periods. Finally, these space methods are illustrated by several interesting case studies that show the best examples of different special phenomena such as long-term amplitude modulation, amplitude decrease and mode switching.

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arXiv1999

Early-time spectroscopic observations of SN 1998aq in NGC 3982

Medium resolution spectroscopic observations of SN 1998aq made in April-May, 1998, are presented. We confirm its Type Ia classification based on the prominent Si II 6355 A line and other features similar to SNe Ia. No significant sign of hydrogen Balmer-alpha line was seen in high-resolution spectra taken at 8 days before maximum. Preliminary estimate of reddening and distance modulus, based on the correlation between the line depth ratio of two Si II features around 6000 A and BVRI light curves of Type Ia SNe, is presented. Moreover, H-alpha emission from the core of the Seyfert 2 type host galaxy NGC 3982 has also been detected.

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arXiv1999

V2109 Cygni, a second overtone field RR Lyrae star

We present the first (as of February, 1999) UBV and uvby photometric measurements for the short period variable star V2109 Cyg discovered by the Hipparcos satellite and classified as a field RRc variable. We have obtained new times of maxima and the period change has been studied. We determined the fundamental physical parameters using the geometric distance of the star and the most recent synthetic colour grids. The results are: [Fe/H]=-0.9+/-0.2, Mbol=0.73+/-0.43 mag, =6800+/-200 K, log g=2.7+/-0.2, R=4.6+/-0.9 Ro. Additionally, we took medium resolution (lambda/Delta lambda=11000) spectra in the red spectral region centered at 6600 A. A complete radial velocity curve has been determined from 60 spectra. We found no systematic difference between the velocities from Halpha and metallic lines indicating a smooth pulsation. The mass of the star is found to be M=0.5+/-0.3 Mo using the photometric log g value and the acceleration curve calculated from the radial velocity data. The finally adopted set of the physical parameters lies in the typical range of RR Lyrae stars, which implies that V2109 Cyg is the shortest period RR Lyrae-type variable. The visual amplitude vs. period and the Fourier amplitude parameter R21} vs. period diagrams suggest that V2109 Cyg probably pulsates in the second overtone mode.

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