IW And-type state in IM Eridani

Katô, Takeo; Wakamatsu, Yasuyuki; Kojiguchi, Naoto; Kimura, M.; Ohnishi, Ryuhei; Isogai, Keisuke; Niijima, Kyo; Yoshitake, T.; Sumiya, Sho; Ito, Daiki; Nikai, Kengo; Matsumoto, Hanami; Matsumoto, Katsura; Vanmunster, Tonny; Hambsch, Franz-Josef; Itoh, Hiroshi; Babina, Julia V.; Antonyuk, Oksana I.; Baklanov, Alex; Павленко, Е. П.; Monard, B.; Dvorak, Shawn

doi:10.1093/pasj/psz130

Cited by 10 publications

(3 citation statements)

References 28 publications

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“…With the exception of V5662 Sgr, the optical light curves are well enough sampled to show that none of our targets were in a low state during our radio observations. Note the IW And-type photometric behaviour discussed by Kato et al (2020) in the light curve of IM Eri. Figure 6.…”

Section: Mass Accretion Ratesmentioning

confidence: 89%

A MeerKAT survey of nearby nova-like cataclysmic variables

Hewitt

Pretorius

Woudt

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT We present the results of MeerKAT radio observations of 11 nearby nova-like cataclysmic variables (CVs). We have detected radio emission from IM Eri, RW Sex, V3885 Sgr, and V603 Aql. While RW Sex, V3885 Sgr, and V603 Aql had been previously detected, this is the first reported radio detection of IM Eri. Our observations have doubled the sample of non-magnetic CVs with sensitive radio data. We observe that at our radio detection limits, a specific optical luminosity ${\gtrsim}2.2\times 10^{18}\,$ erg s−1 Hz−1 (corresponding to MV ≲ 6.0) is required to produce a radio detection. We also observe that the X-ray and radio luminosities of our detected nova-like CVs are on an extension of the $L_X\propto L_R^{\sim 0.7}$ power law originally proposed for non-pulsating neutron star low-mass X-ray binaries. We find no other correlations between the radio emission and emission in other wavebands or any other system parameters for the existing sample of radio-detected non-magnetic CVs. We measure in-band (0.9–1.7 GHz) radio spectral indices that are consistent with reports from earlier work. Finally, we constructed broad spectral energy distributions for our sample from published multiwavelength data, and use them to place constraints on the mass transfer rates of these systems.

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Section: Mass Accretion Ratesmentioning

confidence: 89%

A MeerKAT survey of nearby nova-like cataclysmic variables

Hewitt

Pretorius

Woudt

et al. 2020

Monthly Notices of the Royal Astronomical Society

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show abstract

“…With the exception of V5662 Sgr, the optical light curves are well enough sampled to show that none of our targets were in a low state during our radio observations. Note the IW And-type photometric behaviour discussed byKato et al (2020) in the light curve of IM Eri.…”

mentioning

confidence: 89%

A MeerKAT Survey of Nearby Novalike Cataclysmic Variables

Hewitt,

Pretorius,

Woudt

et al. 2020

Preprint

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We present the results of MeerKAT radio observations of eleven nearby novalike cataclysmic variables. We have detected radio emission from IM Eri, RW Sex, V3885 Sgr and V603 Aql. While RW Sex, V3885 Sgr and V603 Aql had been previously detected, this is the first reported radio detection of IM Eri. Our observations have doubled the sample of non-magnetic CVs with sensitive radio data. We observe that at our radio detection limits, a specific optical luminosity 2.2 × 10 18 erg s −1 Hz −1 (corresponding to M V 6.0) is required to produce a radio detection. We also observe that the X-ray and radio luminosities of our detected NLs are on an extension of the L X ∝ L ∼0.7 R power law originally proposed for non-pulsating neutron star low-mass X-ray binaries. We find no other correlations between the radio emission and emission in other wavebands or any other system parameters for the existing sample of radiodetected non-magnetic CVs. We measure in-band (0.9-1.7 GHz) radio spectral indices that are consistent with reports from earlier work. Finally, we constructed broad spectral energy distributions for our sample from published multi-wavelength data, and use them to place constraints on the mass transfer rates of these systems.

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“…However, despite more than 40 years of extensive research on CVs and more than 1400 systems with a measured orbital period (Ritter & Kolb, 2003), only a handful of period bouncer candidates have been identified so far (e.g. Patterson et al 2005;Unda-Sanzana et al 2008;Littlefair et al 2006;Patterson 2011;Kato et al 2015Kato et al , 2016McAllister et al 2017;Neustroev et al 2017, and many others), therefore enlarging the sample of post-bounce CVs is important in order to validate a fundamental prediction of the current models of compact binary evolution.…”

Section: Introductionmentioning

confidence: 99%