RR Pic (1925): a<i>Chandra</i>X-ray view

Pekön, Yakup; Balman, Ş.

doi:10.1111/j.1365-2966.2008.13467.x

Cited by 4 publications

(4 citation statements)

References 30 publications

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“…During the eclipse, the absorption increases, reducing the emission from the lower end of the flow and hence the lower temperature values increase. The change in absorption over the orbital motion has been encountered before in another CV; a classical nova RR Pic (Pekön & Balman 2008) where an absorbing region on the disk in the line of sight affects the spectrum. This makes the spectral behaviour of CVs over the orbital period an area worth more investigation.…”

Section: Discussionmentioning

confidence: 66%

Orbital and spin phase-resolved spectroscopy of the intermediate polar EX Hya using XMM-Newton data

Pekön

Balman

2010

Monthly Notices of the Royal Astronomical Society

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We present the orbital phase‐resolved spectra of an intermediate polar, EX Hya, together with the spin phase‐resolved spectra during two different epochs using the X‐ray Multi‐Mirror Mission (XMM–Newton), European Photon Imaging Camera (pn instrument). We find that the source at the two epochs has the same X‐ray luminosity of ∼6.5 × 1031 erg s−1. We detect spectral variations between the 2000 and 2003 observations of the source. We fitted the spectrum using a neutral hydrogen absorption model with or without covering fraction together with Gaussians for emission lines, two collisional equilibrium plasma emission models (MEKAL) and a cooling‐flow plasma emission model (VMCFLOW). We find that two of the three emission components (kT= 0.6–0.8 and 1.3–1.7 keV) fitted by the MEKAL models are almost constant over the spin and orbital phases and also over the two different epochs with the normalization varying directly proportional to the flux when the data are folded according to the orbital and spin phase indicating that the slight variation may be due to occultation. The emission modelled by the VMCFLOW changes over the spin and orbital phases and the 2000 and 2003 observations reveal two different ranges of temperatures (3–33 and 8–61 keV, respectively) that model the shock zone in the accretion column(s). The ratios of the spin maximum to minimum and the orbital maximum to minimum spectra along with the increase in the plasma temperatures indicate that the spectrum gets harder in the minimum phases of both orbital and spin periods. In the 2003 observation, a 6.4 keV fluorescent Fe emission line is present at the orbital minima in a range of phases from 0.9 to 1.3 and it is absent otherwise. This indicates that there is reflection from the disc most likely from a large bulge at the accretion impact zone.

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Section: Discussionmentioning

confidence: 66%

Orbital and spin phase-resolved spectroscopy of the intermediate polar EX Hya using XMM-Newton data

Pekön

Balman

2010

Monthly Notices of the Royal Astronomical Society

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“…It is unclear if strong magnetic fields play any role in shaping the outburst or the ejecta of CNe (Livio et al 1988, Nikitin et al 2000. The fact that RR Pic is not an Intermediate Polar (Pekön & Balman 2008), but also has a discrepant nebular expansion parallax, indicates -28that the presence of a strong magnetic field does not appear to dramatically affect the shell ejection process.…”

Section: Discussionmentioning

confidence: 99%

HUBBLE SPACE TELESCOPEFINE GUIDANCE SENSOR PARALLAXES FOR FOUR CLASSICAL NOVAE^,

Harrison

Bornak

McArthur³

et al. 2013

ApJ

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We have used data obtained with the Fine Guidance Sensors on the Hubble Space Telescope to derive precise astrometric parallaxes for four classical novae: V603 Aql, DQ Her, GK Per, and RR Pic. All four objects exceeded the Eddington limit at visual maximum. Re-examination of the original light curve data for V603 Aql and GK Per has led us to conclude that their visual maxima were slightly brighter than commonly assumed. With known distances, we examine the various maximum magnitude−rate of decline (MMRD) relationships that have been established for classical novae. We find that these four objects show a similar level of scatter about these relationships as seen in larger samples of novae whose distances were determined using indirect techniques. We also examine the nebular expansion parallax method, and find that it fails for three of the four objects. In each case it was possible to find an explanation for the failure of that technique to give precise distance estimates. DQ Her appears to suffer from an anomalously high extinction when compared to field stars on its sight line. We suggest that this is likely due to local material, which may also be the source of the IRAS detections of this object.

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“…An orbital period of 3.48 h was identified by Vogt (1975) and the binary inclination is 60 & Diaz (2006). RR Pic was observed using ROSAT and found to be a moderately bright X-ray source (van Teeseling et al 1996) whilst observations made using Chandra show evidence for various emission lines in the X-ray spectrum (Pekon & Balman 2008). The astrometric distance determined using the HST fine guidance sensor is 521 +54 −45 pc (Harrison et al 2013).…”

Section: Appendix A: Background Notes On Individual Sourcesmentioning

confidence: 99%

Distances of cataclysmic variables and related objects derived fromGaiaData Release 1

Ramsay

Schreiber

Gänsicke

et al. 2017

A&A

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We consider the parallaxes of sixteen cataclysmic variables and related objects that are included in the TGAS catalogue, which is part of the Gaia first data release, and compare these with previous parallax measurements. The parallax of the dwarf nova SS Cyg is consistent with the parallax determination made using the VLBI, but with only one of the analyses of the HST Fine Guidance Sensor (FGS) observations of this system. In contrast, the Gaia parallaxes of V603 Aql and RR Pic are broadly consistent, but less precise than the HST/FGS measurements. The Gaia parallaxes of IX Vel, V3885 Sgr, and AE Aqr are consistent with, but much more accurate than the Hipparcos measurements. We take the derived Gaia distances and find that absolute magnitudes of outbursting systems show a weak correlation with orbital period. For systems with measured X-ray fluxes we find that the X-ray luminosity is a clear indicator of whether the accretion disc is in the hot and ionised or cool and neutral state. We also find evidence for the X-ray emission of both low and high state discs correlating with orbital period, and hence the long-term average accretion rate. The inferred mass accretion rates for the nova-like variables and dwarf novae are compared with the critical mass accretion rate predicted by the Disk Instability Model. While we find agreement to be good for most systems there appears to be some uncertainty in the system parameters of SS Cyg. Our results illustrate how future Gaia data releases will be an extremely valuable resource in mapping the evolution of cataclysmic variables.

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RR Pic (1925): aChandraX-ray view

Cited by 4 publications

References 30 publications

Orbital and spin phase-resolved spectroscopy of the intermediate polar EX Hya using XMM-Newton data

Orbital and spin phase-resolved spectroscopy of the intermediate polar EX Hya using XMM-Newton data

HUBBLE SPACE TELESCOPEFINE GUIDANCE SENSOR PARALLAXES FOR FOUR CLASSICAL NOVAE^,

Distances of cataclysmic variables and related objects derived fromGaiaData Release 1

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RR Pic (1925): aChandraX-ray view

Cited by 4 publications

References 30 publications

Orbital and spin phase-resolved spectroscopy of the intermediate polar EX Hya using XMM-Newton data

Orbital and spin phase-resolved spectroscopy of the intermediate polar EX Hya using XMM-Newton data

HUBBLE SPACE TELESCOPEFINE GUIDANCE SENSOR PARALLAXES FOR FOUR CLASSICAL NOVAE,

Distances of cataclysmic variables and related objects derived fromGaiaData Release 1

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HUBBLE SPACE TELESCOPEFINE GUIDANCE SENSOR PARALLAXES FOR FOUR CLASSICAL NOVAE^,