2020
DOI: 10.3847/1538-4357/ab9197
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The Rise and Fall of the King: The Correlation between FO Aquarii’s Low States and the White Dwarf’s Spin-down

Abstract: The intermediate polar FOAquarii (FO Aqr) experienced its first reported low-accretion states in

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Cited by 25 publications
(22 citation statements)
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“…3). Although the ASAS-SN lightcurve indicates that TW Pic can undergo slow transitions from a high to a low state (and vice versa) on timescales of weeks to months as is observed in several other accreting white dwarfs 1,19,20 , the moding behaviour occurring on ≈30 minute timescales appears to be restricted to the more recent observations. The TESS Cycle 3 data also reveal the mode switching from the low to the high mode, occurring on a somewhat longer timescale of ≈12 hours (see Extended Data Fig.…”
mentioning
confidence: 81%
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“…3). Although the ASAS-SN lightcurve indicates that TW Pic can undergo slow transitions from a high to a low state (and vice versa) on timescales of weeks to months as is observed in several other accreting white dwarfs 1,19,20 , the moding behaviour occurring on ≈30 minute timescales appears to be restricted to the more recent observations. The TESS Cycle 3 data also reveal the mode switching from the low to the high mode, occurring on a somewhat longer timescale of ≈12 hours (see Extended Data Fig.…”
mentioning
confidence: 81%
“…This suggests that the optical emission of TW Pic, at that epoch, was due to the bare white dwarf and secondary star photospheres and hence that accretion was turned off. Furthermore, the ROSAT All Sky survey observed TW Pic between Aug. [12][13][14][15][16][17][18][19][20][21][22]1990 and between Feb. [13][14][15]1991. From inspection of the X-ray light curve of TW Pic, provided in the Second ROSAT X-ray Source (2RXS) catalogue products 42 , the source is not significantly detected in August, while it is detected at the 4σ level in February, further supporting that accretion switched off in August 1990.…”
Section: Archival X-ray and Optical Observations Of Tw Picmentioning
confidence: 99%
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“…IPs have spin periods of order minutes to tens of minutes (Patterson 1994). These are rates much slower than breakup, but faster than their binary periods, reflecting a quasi-equilibrium between spin-up and magnetic drag that is con-tinuously adjusting to a fluctuating accretion rate (Patterson 1984;Kennedy et al 2016;Littlefield et al 2020) Not all systems exist in quasi-equilibrium. One of the first recognised cataclysmic variables, AE Aquarii, shows remarkable flaring behaviour that is thought to be driven by magnetically-propelled material exiting the system (Wynn et al 1997).…”
Section: Introductionmentioning
confidence: 99%
“…The mode of accretion in a particular IP can change in response to variations in the system's mass-transfer rate (M  ). FO Aqr, which shows disk-fed accretion when M  is highest and some form of stream-fed accretion when M  decreases (Littlefield et al 2020), is perhaps the best example of this phenomenon. Overall, disk-fed accretion tends to be the most commonly observed mode of accretion in the majority of IPs.…”
Section: Introductionmentioning
confidence: 99%