On the close optical companion of V1494 Aql:  Problems with
light curve modelling

Kiss, L. L.; Csák, B.; Derekas, A.

doi:10.1051/0004-6361:20034580

Cited by 4 publications

(14 citation statements)

References 10 publications

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“…These observations were made when V1494 Aql was still bright. We see no evidence for contamination of the spectra by features from the nearby G‐type star, as seen at later times by Kiss, Csák & Derekas (2004).…”

Section: Observationsmentioning

confidence: 55%

Six months of mass outflow and inclined rings in the ejecta of V1494 Aql

Eyres

Heywood

O’Brien

et al. 2005

Monthly Notices of the Royal Astronomical Society

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V1494 Aql was a very fast nova which reached a visual maximum of about 4.0 by the end of 1999 December 3. We report observations from 4 to 284 days after discovery, including sub-mm- and cm-band fluxes, a single MERLIN image, and optical spectroscopy in the 410 to 700 nm range. The extent of the radio continuum emission is consistent with a recent lower distance estimate of 1.6 kpc. We conclude that the optical and radio emission arises from the same expanding ejecta. We show that these observations are not consistent with simple kinematical spherical shell models used in the past to explain the rise and fall of the radio flux density in these objects. The resolved remnant structure is consistent with an inclined ring of enhanced density within the ejecta. Optical spectroscopy indicates likely continued mass ejection for over 195 days, with the material becoming optically thin in the visible sometime between 195 and 285 days after outburst.Comment: 6 pages including 3 figure

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Section: Observationsmentioning

confidence: 55%

Six months of mass outflow and inclined rings in the ejecta of V1494 Aql

Eyres

Heywood

O’Brien

et al. 2005

Monthly Notices of the Royal Astronomical Society

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“…Our next case study was inspired by the independent discovery of the close optical companion of nova V1494 Aql (Kiss et al 2004). We selected several bright nova outbursts in the last decade for which progenitor star candidates have been identified in Digitized Sky Survey plates or deep star catalogues (most often in the USNO A1.0 and A2.0 catalogue releases).…”

Section: Field Star Distributions Around Seven Recent Novaementioning

confidence: 99%

“…Interestingly, for V1494 Aql this is also supported by our knowledge of the optical companion. In Kiss et al (2004), we assigned late F‐early G as an approximate spectral type of the companion. The corresponding absolute magnitude for a main‐sequence star is approximately M V =+4.0 mag, which agrees within the error bars with the quiescent absolute magnitude of the nova (Kiss et al 2004).…”

Section: Field Star Distributions Around Seven Recent Novaementioning

confidence: 99%

“…In Kiss et al (2004), we assigned late F‐early G as an approximate spectral type of the companion. The corresponding absolute magnitude for a main‐sequence star is approximately M V =+4.0 mag, which agrees within the error bars with the quiescent absolute magnitude of the nova (Kiss et al 2004). Hence, the close apparent magnitudes of the pre‐nova and the companion suggest similar distances, consequently the possibility of physical correlation.…”

Section: Field Star Distributions Around Seven Recent Novaementioning

confidence: 99%

“…For instance, wide‐field photometric surveys of the galactic field are characterized by confusion radii of 10–20 arcsec (Brown 2003) and can suffer from strong blending, even in regions far from the Galactic plane. Other examples include the presence of a close optical companion of the classical nova V1494 Aql (at a separation of approximately 1.5 arcsec), which heavily affected late light curves of the eclipsing system (Kiss, Csák & Derekas 2004).…”

Section: Introductionmentioning

confidence: 99%

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Photometric biases as a result of stellar blending: implications for measuring distances, constraining binarity and detecting exoplanetary transits

Kiss

Bedding

2005

Monthly Notices of the Royal Astronomical Society

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We investigate blending, binarity and photometric biases in crowded‐field CCD imaging. For this, we consider random blend losses, which correspond to the total number of stars left undetected in unresolved blends. We present a simple formula to estimate blend losses, which can be converted to apparent magnitude biases using the luminosity function (LF) of the analysed sample. Because of the assumptions used, our results give lower limits of the total bias and we show that in some cases even these limits point towards significant limitations in measuring apparent brightnesses of standard candle stars and thus distances to nearby galaxies. A special application is presented for the OGLE‐II BVI maps of the Large Magellanic Cloud (LMC). We find a previously neglected systematic bias up to 0.2–0.3 min for faint stars (V∼ 18.0 –19.0 min) in the OGLE‐II sample, which affects LMC distance measurements using RR Lyrae and red clump stars. We also consider the effects of intrinsic stellar correlations, i.e. binarity, via calculating two‐point correlation functions for stellar fields around seven recently exploded classical novae. In two cases, for V1494 Aql and V705 Cas, the reported close optical companions seem to be physically correlated with the cataclysmic systems. Finally, we find significant blend frequencies up to 50–60 per cent in the samples of wide‐field exoplanetary surveys, which suggests that blending calculations are highly advisable to be included into the regular reduction procedure.

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Detection of Two-armed Spiral Shocks on the Accretion Disk of the Eclipsing Fast Nova V1494 Aquilae

Hachisu

Kato

Katô

2004

ApJ

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We have modeled the unusual orbital light curve of V1494 Aquilae (Nova Aquilae 1999 No.2) and found that such an unusual orbital light curve can be reproduced when there exist two-armed, spiral shocks on the accretion disk. V1494 Aql is a fast classical nova and found to be an eclipsing system with the orbital period of 0.1346138 days in the late phase of the nova outburst. Its orbital light curve shows a small bump at orbital phase 0.2, a small dip at 0.3, sometimes a small bump at 0.4, and a large bump at 0.6 − 0.7 outside eclipse. Such a double-or triple-wave pattern outside eclipse has never been observed even though overall patterns look like some supersoft X-ray sources or eclipsing polars. We have calculated orbital light curves including the irradiation effects of the accretion disk and the companion by the hot white dwarf. These unusual patterns can be reproduced when we assume twoarmed spiral shocks on the accretion disk. Especially, triple-wave patterns are naturally obtained. This result strongly suggests the existence of two-armed spiral shocks on the accretion disk in the late phase of the nova outburst.

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On the close optical companion of V1494 Aql: Problems with light curve modelling

Cited by 4 publications

References 10 publications

Six months of mass outflow and inclined rings in the ejecta of V1494 Aql

Six months of mass outflow and inclined rings in the ejecta of V1494 Aql

Photometric biases as a result of stellar blending: implications for measuring distances, constraining binarity and detecting exoplanetary transits

Detection of Two-armed Spiral Shocks on the Accretion Disk of the Eclipsing Fast Nova V1494 Aquilae

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