The biological transmission of potato leafroll virus by Myzus persicae

Ponsen, M.B.

doi:10.1007/bf01976581

Cited by 12 publications

(8 citation statements)

References 7 publications

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“…An exhaustive list of photometric measurements of ρ Pup was reported by Moon & van Antwerpen (2009). Ponsen (1963), Eggen (1956), and Hipparcos (ESA 1997) data are the most suitable for a detailed analysis. Data were obtained in different passbands: Ponsen's measurements were taken through a blue filter, Eggen's through a yellow filter, and those of Hipparcos in the wide H p passband.…”

Section: ρ Pupmentioning

confidence: 99%

“…The variability of ρ Pup ≡ HD 67523 ≡ HR 3185, one of the brightest (V = 2.88) δ Sct stars, was first reported by Cousins (1951) and then clearly demonstrated by Eggen (1956) and Ponsen (1963). An accurate value of the pulsational period (P = 0.14088143 d) was determined from photometric data spanning fifty-two years (Moon & van Antwerpen 2009).…”

Section: Introductionmentioning

confidence: 96%

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Understanding the dynamical structure of pulsating stars

Nardetto

Poretti

Rainer

et al. 2014

A&A

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Context. High-resolution spectroscopy is a powerful tool to study the dynamical structure of a pulsating star's atmosphere. Aims. We aim at comparing the line asymmetry and velocity of the two δ Sct stars ρ Pup and DX Cet with previous spectroscopic data obtained on classical Cepheids and β Cep stars. Methods. We obtained, analysed and discuss HARPS high-resolution spectra of ρ Pup and DX Cet. We derived the same physical quantities as used in previous studies, which are the first-moment radial velocities and the bi-Gaussian spectral line asymmetries. Results. The identification of f = 7.098 d −1 as a fundamental radial mode and the very accurate Hipparcos parallax promote ρ Pup as the best standard candle to test the period-luminosity relations of δ Sct stars. The action of small-amplitude nonradial modes can be seen as well-defined cycle-to-cycle variations in the radial velocity measurements of ρ Pup. Using the spectral-line asymmetry method, we also found the centre-of-mass velocities of ρ Pup and DX Cet, V γ = 47.49 ± 0.07 km s −1 and V γ = 25.75 ± 0.06 km s −1 , respectively. By comparing our results with previous HARPS observations of classical Cepheids and β Cep stars, we confirm the linear relation between the atmospheric velocity gradient and the amplitude of the radial velocity curve, but only for amplitudes larger than 22.5 km s −1 . For lower values of the velocity amplitude (i.e., <22.5 km s −1 ), our data on ρ Pup seem to indicate that the velocity gradient is null, but this result needs to be confirmed with additional data. We derived the Baade-Wesselink projection factor p = 1.36 ± 0.02 for ρ Pup and p = 1.39 ± 0.02 for DX Cet. We successfully extended the period-projection factor relation from classical Cepheids to δ Scuti stars.

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Section: ρ Pupmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

Understanding the dynamical structure of pulsating stars

Nardetto

Poretti

Rainer

et al. 2014

A&A

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“…The detected minima were separated by about 0.82 d. This prompted de Kort (1955) to do photometry with the Riverview Observatory (Australia) plates. He found that the orbit is highly eccentric and the true orbital period amounts to about 3.28 d. This finding was confirmed by Ponsen (1956). In a survey of spectra of southern eclipsing binaries at Mount Stromlo Observatory, the star was found to be SB2 by Popper (1966).…”

Section: Appendix A: Notes On Individual Starsmentioning

confidence: 76%

Massive heartbeat stars from TESS. I. TESS sectors 1-16

Kołaczek-Szymański,

Pigulski,

Michalska

et al. 2020

Preprint

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Context. Heartbeat stars are eccentric binaries exhibiting characteristic shape of brightness changes during periastron passage caused primarily by variable tidal distortion of the components. Variable tidal potential can drive tidally excited oscillations (TEOs), which are usually gravity modes. Studies of heartbeat stars and TEOs open a new possibility to probe interiors of massive stars. There are only a few massive (masses of components 2 M ) systems of this type known. Aims. Using TESS data from the first 16 sectors, we searched for new massive heartbeat stars and TEOs using a sample of over 300 eccentric spectroscopic binaries. Methods. We analysed TESS 2-min and 30-min cadence data. Then, we fitted Kumar's analytical model to the light curves of stars showing heartbeats and performed times-series analysis of the residuals searching for TEOs and periodic intrinsic variability. Results. We found 20 massive heartbeat systems, of which seven show TEOs. The TEOs occur at harmonics of orbital frequencies in the range between 3 and 36, with the median value equal to 9, lower than those in known Kepler systems with TEOs. The most massive system in this sample is the quadruple star HD 5980, a member of Small Magellanic Cloud. With the total mass of ∼150 M it is the most massive system showing a heartbeat. Six stars in the sample of the new heartbeat stars are eclipsing. Comparison of the parameters derived from fitting Kumar's model and from light-curve modelling shows that Kumar's model does not provide reliable parameters. In other words, orbital parameters can be reliably derived from fitting heartbeat light curves only if model includes all proximity effects. Finally, intrinsic pulsations of β Cep, SPB, δ Sct, and γ Dor-type were found in nine heartbeat systems. This opens an interesting possibility of studies of pulsation-binarity interaction and the co-existence of forced and self-excited oscillations.

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“…The star V703 Sco (HD 160589) is a HADS with periods of P 1 = 0.14996 d (ν 1 = 6.66844 d −1 ), P 2 = 0.11522 d (ν 2 = 6.67905 d −1 ), which might be due to the fundamental and first overtone modes, with a ratio of 0.768, and (Ponsen, 1961;Oosterhoff, 1966;Koen, 2001). The rotational velocity is v sin i = 16 km s −1 and the spectral type is A9V (Houk, 1982).…”

Section: V703 Sco and 1 Monmentioning

confidence: 99%

Near infrared spectroscopy of the HADS stars V703 Sco and 1 Mon: First steps towards the use of near-IR spectroscopy for the study of δ Scuti stars

Amado¹

2007

cia

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Intermediate results from an ongoing programme to study the possibilities of near-infrared spectroscopy are presented for the always difficult task of providing information on the mode identification of pulsating stars. High-resolution spectroscopy taken with crires shows, for the first time, stellar absorption lines in the near-IR varying with the pulsation cycle in the high amplitude δ Scuti star 1 Mon. 1 1 Based on observations collected at the European Southern Observatory at La Silla and Paranal, Chile (crires science verification program 60.A-9086

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The biological transmission of potato leafroll virus by Myzus persicae

Cited by 12 publications

References 7 publications

Understanding the dynamical structure of pulsating stars

Understanding the dynamical structure of pulsating stars

Massive heartbeat stars from TESS. I. TESS sectors 1-16

Near infrared spectroscopy of the HADS stars V703 Sco and 1 Mon: First steps towards the use of near-IR spectroscopy for the study of δ Scuti stars

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