The symbiotic binary <scp>ZZ CMi</scp>: Intranight variability and suggested outbursting nature

Zamanov, R.; Stoyanov, K. A.; Kostov, A.; Kurtenkov, A.; Nikolov, Geno; Latev, G.; Bode, M. F.; Martı́, Josep; Luque-Escamilla, Pedro L.; Tomov, N. A.; Nikolov, Y.; Boeva, S.

doi:10.1002/asna.202113975

Cited by 6 publications

(7 citation statements)

References 34 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Ground-based observations in the B filter by Zamanov et al (2016a) revealed a flickering amplitude of 0.08 mag in February 2016. Subsequent observations from January to August 2023 detected variability in the range of 0.11-0.26 mag (Shore & Teyssier 2023;Minev et al 2023;Zamanov et al 2023a). This observed variability aligns broadly with the anticipated B amplitudes inferred from the TESS observations.…”

Section: Detection Of Flickering With Tesssupporting

confidence: 56%

“…The challenge lies in the small amplitude of optical flickering and the limitations of relatively small ground-based telescopes used for such searches. Furthermore, even in cases where flickering is undoubtedly detected, it may not be present at all epochs (e.g., Lucy et al 2020;Georgiev et al 2022;Zamanov et al 2023b;Pujol et al 2023). Therefore, it is necessary to obtain observations over an extended period of time.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Accretion-induced flickering variability among symbiotic stars from space photometry with NASA TESS

Merc,

Beck,

Mathur

et al. 2024

A&A

View full text Add to dashboard Cite

Symbiotic binaries exhibit a wide range of photometric variability across different timescales. These changes can be attributed to factors such as orbital motion, intrinsic variability of the individual components, or interactions between the two stars. In the range from minutes to hours, a variability induced by accretion processes that is likely to originate from the accretion disks has been detected and subsequently denoted as flickering. This variability could mimic solar-like oscillations exhibited by luminous red giants. We aim to investigate whether it is possible to utilize the precise observations of the NASA TESS mission to detect flickering in symbiotic stars, despite the fact that such studies are usually performed at shorter wavelengths than those of TESS observations. Additionally, our goal is to develop a quantitative method for the detection of accretion-induced flickering that does not rely solely on a subjective assessment of the light curves. We obtained the light curves of known symbiotic stars and a comprehensive control sample of assumed single red giants from the TESS full-frame images. To ensure consistency, all the data were processed using the same methodology, which involves filtering out the background, systematic, and long-term trends. From the processed light curves and their power spectral densities, we measured the amplitudes of the variability and other relevant parameters. We introduce a method that enables a differentiation between flickering sources and stars that do not exhibit this type of variability. We detected flickering-like variability in 20 symbiotic stars utilizing TESS data, of which 13 had not previously been identified as flickering sources. Moreover, the TESS observations facilitate the detection of related variations occurring over timescales of a few days, as well as changes in the flickering behavior across multiple sectors. The flickering is now likely to be detected in a total of 35 known symbiotic stars. While this represents only a small subset of all symbiotic binaries, when focusing solely on accreting-only symbiotic stars where the detection of flickering is presumably more straightforward, the fraction could reach as high as sim \,80<!PCT!>. This result suggests that accretion disks may indeed be prevalent in these binaries.

show abstract

Section: Detection Of Flickering With Tesssupporting

confidence: 56%

Section: Introductionmentioning

confidence: 99%

Accretion-induced flickering variability among symbiotic stars from space photometry with NASA TESS

Merc,

Beck,

Mathur

et al. 2024

A&A

View full text Add to dashboard Cite

show abstract

“…Similarly, while large amplitude flickering has always been the rule for MWC 560 (eg. Lucy et al 2020), it has disappeared altogether during the last couple of years (Zamanov et al 2019).…”

Section: Optical Flickeringmentioning

confidence: 99%

The GALAH Survey and Symbiotic Stars. I. Discovery and follow-up of 33 candidate accreting-only systems

Munari,

Traven,

Masetti

et al. 2021

Preprint

View full text Add to dashboard Cite

We have identified a first group of 33 new candidates for symbiotic stars (SySt) of the accretingonly variety among the 600 255 stars so far observed by the GALAH high-resolution spectroscopic survey of the Southern Hemisphere, more than doubling the number of those previously known. GALAH aims to high latitudes and this offers the possibility to sound the Galaxy for new SySt away from the usual Plane and Bulge hunting regions. In this paper we focus on SySt of the M spectral type, showing an H emission with a peak in excess of 0.5 above the adjacent continuum level, and not affected by coherent radial pulsations. These constraints will be relaxed in future studies. The 33 new candidate SySt were subjected to a vast array of follow-up confirmatory observations (X-ray/UV observations with the Swift satellite, search for optical flickering, presence of a near-UV upturn in ground-based photometric and spectroscopic data, radial velocity changes suggestive of orbital motion, variability of the emission line profiles). According to Gaia DR3 parallaxes, the new SySt are located at the tip of the Giant Branch, sharing the same distribution in M(K ) of the well established SySt. The accretion luminosities of the new SySt are in the range 1−10 L ⊙ , corresponding to mass-accretion rates of 0.1-1 10 −9 M ⊙ yr −1 for WDs of 1 M ⊙ . The M giant of one of the new SySt presents a large Lithium over-abundance.

show abstract

“…This prompted a flurry of observations across the electromagnetic spectrum, from very high energy TeV/GeV γ-rays detected by H.E.S.S. 3 (Wagner 2021a,b;Aharonian et al 2022) and MAGIC 4 (Acciari et al 2022), and MeV γrays by Fermi-LAT 5 (Cheung et al 2021a(Cheung et al ,b, 2022; to X-rays seen by MAXI 6 (Shidatsu et al 2021), INTE-GRAL 7 (Ferrigno et al 2021), NICER 8 (Enoto et al 2021a,b;Luna et al 2021;Orio et al 2021b,c), NuS-TAR 9 (Luna et al 2021), AstroSat (Rout et al 2021), Chandra and XMM-Newton (Orio et al 2021a), as well as Swift (Page, Osborne & Aydi 2021;Page 2021a,b); to optical (Taguchi, Ueta & Isogai 2021;Munari & Valisa 2021a;Mikolajewska et al 2021;Munari & Valisa 2021b;Nikolov & Luna 2021;Shore et al 2021a;Shore, Teyssier & Thizy 2021;Shore et al 2021b;Munari, Valisa & Ochner 2021;Fajrin et al 2021;Ricra, Vannini & Baella 2021;Zamanov et al 2021); infrared (Woodward et al 2021a,b); and radio (Williams et al 2021;Sokolovsky et al 2021;Peters et al 2021). A neutrino search was performed by IceCube, though only upper limits could be placed (Pizzuto, Vandenbroucke & Santander 2021).…”

Section: Introductionmentioning

confidence: 99%

The 2021 outburst of the recurrent nova RS Ophiuchi observed in X-rays by the Neil Gehrels Swift Observatory: a comparative study

Page,

Beardmore,

Osborne

et al. 2022

Preprint

View full text Add to dashboard Cite

On 2021 August 8, the recurrent nova RS Ophiuchi erupted again, after an interval of 15.5 yr. Regular monitoring by the Neil Gehrels Swift Observatory began promptly, on August 9.9 (0.37 day after the optical peak), and continued until the source passed behind the Sun at the start of November, 86 days later. Observations then restarted on day 197, once RS Oph emerged from the Sun constraint. This makes RS Oph the first Galactic recurrent nova to have been monitored by Swift throughout two eruptions. Here we investigate the extensive X-ray datasets from 2006 and 2021, as well as the more limited data collected by EXOSAT in 1985. The hard X-rays arising from shock interactions between the nova ejecta and red giant wind are similar following the last two eruptions. In contrast, the early supersoft source (SSS) in 2021 was both less variable and significantly fainter than in 2006. However, 0.3-1 keV light-curves from 2021 reveal a 35 s quasi-periodic oscillation consistent in frequency with the 2006 data. The Swift X-ray spectra from 2021 are featureless, with the soft emission typically being well parametrized by a simple blackbody, while the 2006 spectra showed much stronger evidence for superimposed ionized absorption edges. Considering the data after day 60 following each eruption, during the supersoft phase the 2021 spectra are hotter, with smaller effective radii and lower wind absorption, leading to an apparently reduced bolometric luminosity. We explore possible explanations for the gross differences in observed SSS behaviour between the 2006 and 2021 outbursts.

show abstract

The symbiotic binary ZZ CMi: Intranight variability and suggested outbursting nature

Cited by 6 publications

References 34 publications

Accretion-induced flickering variability among symbiotic stars from space photometry with NASA TESS

Accretion-induced flickering variability among symbiotic stars from space photometry with NASA TESS

The GALAH Survey and Symbiotic Stars. I. Discovery and follow-up of 33 candidate accreting-only systems

The 2021 outburst of the recurrent nova RS Ophiuchi observed in X-rays by the Neil Gehrels Swift Observatory: a comparative study

Contact Info

Product

Resources

About