IUE and other new observations of the slow nova RR Tel

Penston, M. V.; Benvenuti, P.; Cassatella, A.; Heck, André; Selvelli, P. L.; Macchetto, F.; Ponz, D.; Jordan, C.; Cramer, N.; Rufener, F.; Manfroid, Jean

doi:10.1093/mnras/202.3.833

Cited by 97 publications

(115 citation statements)

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“…Thus, in determining the distance to the star, one should take into account the fact that the extinction in the direction of the cool component includes circumstellar as well as interstellar extinction. The interstellar extinction towards RR Tel is E(B − V) = 0.10−0.11 (Penston et al 1983;Young et al 2005) which would give A K ∼ 0.03 mag.…”

Section: Distance Estimatesmentioning

confidence: 96%

“…Since its nova-like optical outburst in 1944 long term spectroscopic and photometric observations have been carried out in the UV, optical and IR spectral regions in order to establish a satisfactory model of this puzzling object. Inter-comparison of data from observations in different wavelength regions made a significant contribution to these attempts (Heck & Manfroid 1985;Contini & Formiggini 1999;Penston et al 1983;Whitelock 1987).…”

Section: Introductionmentioning

confidence: 99%

“…The distance of RR Tel is not well defined, estimates of it ranging between about 2.5 kpc (Thackeray 1977;Penston et al 1983) to 3.6 kpc . By use of more recent material and with the considerably increased amount of observational IR data for RR Tel and other symbiotic Miras, we give a revised distance estimate for RR Tel.…”

Section: Introductionmentioning

confidence: 99%

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The effect of dust obscuration in RR Telescopii on optical and IR long-term photometry and Fe II emission lines

Kotnik-Karuza¹,

Friedjung²,

Whitelock³

et al. 2006

A&A

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Aims. Infrared and optical photometric and spectroscopic observations of the symbiotic nova RR Tel are used to study the effects and properties of dust in symbiotic binaries containing a cool Mira component, as well as showing "obscuration events" of increased absorption, which are typical for such Miras. Results. We discuss the three periods during which the Mira component was heavily obscured by dust as observed in the different wavelength bands. A change in the correlations of J with other infrared magnitudes was observed with the colour becoming redder after JD 2 446 600. Generally, J−K was comparable, while K −L was larger than typical values for single Miras. A distance estimate of 2.5 kpc, based on the IR data, is given. A larger flux decrease for the permitted than for the forbidden Fe II lines, during the obscuration episode studied, has been found. There is no evidence for other correlations with line properties, in particular with wavelength, which suggests obscuration due to separate optically thick clouds in the outer layers. Conclusions.

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Section: Distance Estimatesmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

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The effect of dust obscuration in RR Telescopii on optical and IR long-term photometry and Fe II emission lines

Kotnik-Karuza¹,

Friedjung²,

Whitelock³

et al. 2006

A&A

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“…Although it is one of the most studied symbiotic systems, many of the physical parameters defining RR Tel are still uncertain, including the orbital period of the system. A better understanding of this system is needed in order to understand its extraordinarily diverse and rich emission line spectrum (Penston et al 1983). RR Tel is one of the few known symbiotic novae, it erupted in 1945.…”

Section: Rr Telmentioning

confidence: 99%

Modeling of C IV pumped fluorescence of Fe II in symbiotic stars

Eriksson

Nilsson

Veenhuizen³

et al. 2007

A&A

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Aims. We describe how the C iv λ1548.18 line pumps the 1548.20 and 1548.41 Å channels of Fe ii in symbiotic stars through the process known as photo-ionization by accidental resonance (PAR). We describe where and why Fe ii fluorescence arises in symbiotic stars and whether the Fe ii λ1548.41 channel can only be activated when there is a white-dwarf wind present in the system. Further, we aim to show how an analysis of the PAR-pumped lines helps to understand the phyisical conditions that they manifest.Methods. We calculate intensities of the C iv-pumped Fe ii fluorescence lines in symbiotic stars, corresponding to the y 4 H 11/2 and w 2 D 3/2 levels, based on a simple geometrical model of the emitting regions. We apply the model to seven symbiotic stars, known to have Fe ii fluorescence lines pumped by C iv in their spectra. We compare the predicted intensities to the observed intensities of the selected symbiotic stars. Results. We find that we can reproduce the observed fluorescence intensities of the seven symbiotic stars in our sample, using parameters that are consistent with their known properties. We show that PAR-produced lines can be used as a diagnostic tool to derive important physical parameters of a stellar system. We suggest that the detection of Fe ii lines corresponding to the w 2 D 3/2 level in certain symbiotic stars provide evidence of hot shells expanding with velocities of at least hundreds km s −1 in those systems.

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“…Examples can be seen in Selvelli & Bonifacio (2000) and Selvelli et al (2007). Penston et al (1983) made a thorough study of the IUE spectrum of RR Tel, where they identified more than 400 emission lines in the UV range. Harper et al (1999) used HST Goddard High Resolution Spectrograph (GHRS) spectra to provide constraints to atomic data for O IV.…”

Section: Introductionmentioning

confidence: 99%

XMM-Newtonobservations of RR Telescopii: evidence for wind signatures and shocked gas emission

González‐Riestra

Selvelli

Cassatella

2013

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RR Telescopii is the prototype of the symbiotic novae class. Since its outburst in 1944, it has been slowly fading, and its emission-line spectrum has evolved significantly. In this paper we discuss XMM-Newton observations of RR Tel taken in April 2009. These are the first X-ray high-resolution spectra of this system, and they provide important information about the physical conditions of the emitting gas. We have estimated the temperature and the luminosity of the hot star to be 154 kK and 5000 L , respectively, from the comparison of model atmospheres with the X-ray spectra. Normalisation of the models with the far ultraviolet flux leads to similar values. Both the shape of the low-resolution X-ray spectrum and the spectral diagnostics that make use of the emission lines present in the RGS spectrum indicate the existence of collisionally ionised gas. At least two components are present, with temperatures of ≈0.6 and 1.7 MK. The existence of a wind from the hot star is unequivocally confirmed by HST-STIS observations taken in 2000, which showed displaced absorption components for the N V 1240 Å and C IV 1550 Å doublets. These components have terminal velocities of the order of 400 km s −1 , which is consistent with the temperature of the gas detected in X-rays.

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IUE and other new observations of the slow nova RR Tel

Cited by 97 publications

References 0 publications

The effect of dust obscuration in RR Telescopii on optical and IR long-term photometry and Fe II emission lines

The effect of dust obscuration in RR Telescopii on optical and IR long-term photometry and Fe II emission lines

Modeling of C IV pumped fluorescence of Fe II in symbiotic stars

XMM-Newtonobservations of RR Telescopii: evidence for wind signatures and shocked gas emission

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