YETI observations of the young transiting planet candidate CVSO 30 b

Raetz, St.; Schmidt, T. O. B.; Czesla, S.; Klocová, T.; Holmes, Lewis M.; Errmann, R.; Kitze, M.; Fernández, M.; Sota, A.; Hernández, Jesús; Downes, Juan José; Dimitrov, D.; Kjurkchieva, D.; Radeva, V.; Wu, Zhen; Zhou, Xin; Takahashi, H.; Henych, T.; Seeliger, Martin; Mugrauer, M.; Adam, Ch.; Marka, C.; Schmidt, J.; Hohle, M. M.; Ginski, C.; Pribulla, T.; Trepl, L.; Moualla, M.; Pawellek, N.; Gelszinnis, Jakob; Buder, Sven; Masda, Suhail G.; Maciejewski, G.; Neuhäuser, R.

doi:10.1093/mnras/stw1159

Cited by 41 publications

(33 citation statements)

References 51 publications

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“…Although once the planetary hypothesis had no edge, Raetz et al (2016) and Johns-Krull et al (2016b) supported the presence of a disintegrating planet. The former monitored for three years and could not confirm the shrinking period reported in Yu et al (2015).…”

Section: Introductionmentioning

confidence: 99%

“…Yu et al (2015), table B1 inRaetz et al (2016), and table 1 inOnitsuka et al (2017) to plot. Note that the data observed byvan Eyken et al (2012) were taken from table 1 inYu et al (2015) and only "complete" data inRaetz et al (2016) were employed.In the top panel, there is a sequence from data observed by vanEyken et al (2012) to dip-B. Then, assuming that they have the same source and dip-A has a different origin from dip-B, new ephemeris was derived using only dip-B in our data.…”

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confidence: 99%

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Evidence for planetary hypothesis for PTFO 8-8695 b with five-year optical/infrared monitoring observations

Tanimoto

Yamashita

et al. 2020

Publications of the Astronomical Society of Japan

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PTFO 8-8695 b (CVSO 30 b) is a young planet candidate whose host star is a ∼ 2.6 Myr-old T-Tauri star, and there have been continuous discussions about the nature of this system. To unveil the mystery of this system, we observed PTFO 8-8695 for around five years at optical and infrared bands simultaneously using Kanata telescope at the Higashi-Hiroshima Observatory. Through our observations, we found that the reported fading event split into two: deeper but phase-shifted "dip-A" and shallower but equiphase "dip-B". These dips disappeared at different epochs, and then, dip-B reappeared. Based on the observed wavelength dependence of dip depths, a dust clump and a precessing planet are likely origins of dip-A and B, respectively. Here we propose "a precessing planet associated with a dust cloud" scenario for this system. This scenario is consistent with the reported change in the depth of fading events, and even with the reported results, which were thought to be negative evidence to the planetary hypothesis, such as the past non-detection of the Rossiter-McLaughlin effect. If this scenario is correct, this is the third case of a young (< 3 Myr) planet around a pre-main sequence star. This finding implies that a planet can be formed within a few Myr.

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Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

Evidence for planetary hypothesis for PTFO 8-8695 b with five-year optical/infrared monitoring observations

Tanimoto

Yamashita

et al. 2020

Publications of the Astronomical Society of Japan

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“…In the nomenclature used by Yu et al (2015), the covered epochs are −690 and −689 4 . The ephemerides given by van Eyken et al (2012) show fading event times preceding those predicted by Raetz et al (2016) by about 2 ks. The formal (statistical) uncertainty of the fading event times is 0.6 ks in the case of Yu et al (2015) and 0.1 ks in the case of Raetz et al (2016).…”

Section: X-ray Photometrymentioning

confidence: 69%

“…The ephemerides given by van Eyken et al (2012) show fading event times preceding those predicted by Raetz et al (2016) by about 2 ks. The formal (statistical) uncertainty of the fading event times is 0.6 ks in the case of Yu et al (2015) and 0.1 ks in the case of Raetz et al (2016). As the earliest photometric data published by van Eyken et al (2012) were obtained in Dec. 2009 (i.e., about six months after the XMM-Newton observations), all calculations of the fading event times require extrapolation.…”

Section: X-ray Photometrymentioning

confidence: 69%

“…2 we also show our definition of the flaring period, which starts at MJD 54 891.847 and lasts for 17 ks. Given that the stellar rotation period is almost identical to or slightly larger than the planetary orbital period of 39.7 ks (van Eyken et al Raetz et al 2016), the flare lasts for essentially half a stellar rotation period. Even so, the flare light curve shows no evidence of an occultation of the flare region by the star.…”

Section: X-ray Photometrymentioning

confidence: 96%

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X-ray emission in the enigmatic CVSO 30 system

Czesla

Schneider

Salz

et al. 2019

A&A

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CVSO 30 is a young, active, weak-line T Tauri star; it possibly hosts the only known planetary system with both a transiting hot-Jupiter and a cold-Jupiter candidate (CVSO 30 b and CVSO 30 c). We analyzed archival ROSAT, Chandra, and XMM-Newton data to study the coronal emission in the system. According to our modeling, CVSO 30 shows a quiescent X-ray luminosity of ≈ 8 × 10 29 erg s −1 . The X-ray absorbing column is consistent with interstellar absorption. XMM-Newton observed a flare, during which a transit of the candidate CVSO 30 b was expected, but no significant transit-induced variation in the X-ray flux is detectable. While the hot-Jupiter candidate CVSO 30 b has continuously been undergoing mass loss powered by the high-energy irradiation, we conclude that its evaporation lifetime is considerably longer than the estimated stellar age of 2.6 Myr.1 van Eyken et al. (2012) actually dubbed them transits; here we adopt the nomenclature also used by Yu et al. (2015).

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Low-Mass and Sub-stellar Eclipsing Binaries in Stellar Clusters

Lodieu

Paunzen

Zejda

2020

Reviews in Frontiers of Modern Astrophysics

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We highlight the importance of eclipsing double-line binaries in our understanding on star formation and evolution. We review the recent discoveries of low-mass and sub-stellar eclipsing binaries belonging to star-forming regions, open clusters, and globular clusters identified by ground-based surveys and space missions with highresolution spectroscopic follow-up. These discoveries provide benchmark systems with known distances, metallicities, and ages to calibrate masses and radii predicted by state-of-the-art evolutionary models to a few percent. We report their density and discuss current limitations on the accuracy of the physical parameters. We discuss future opportunities and highlight future guidelines to fill gaps in age and metallicity to improve further our knowledge of low-mass stars and brown dwarfs.

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YETI observations of the young transiting planet candidate CVSO 30 b

Cited by 41 publications

References 51 publications

Evidence for planetary hypothesis for PTFO 8-8695 b with five-year optical/infrared monitoring observations

Evidence for planetary hypothesis for PTFO 8-8695 b with five-year optical/infrared monitoring observations

X-ray emission in the enigmatic CVSO 30 system

Low-Mass and Sub-stellar Eclipsing Binaries in Stellar Clusters

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