Long-term monitoring and interpretation of flares in the H2O maser emission of IRAS 16293–2422

Colom, P.; Lekht, E. E.; Pashchenko, M. I.; Rudnitskii, G. M.; Толмачев, А. М.

doi:10.1134/s1063772916080059

Cited by 7 publications

(16 citation statements)

References 22 publications

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“…OD has also been discovered on these scales with SOFIA (Parise et al 2012). OH has been observed at cm wavelengths and its emission appears to have variable flares (Colom et al 2016).…”

Section: C123 Glycine (Nh2ch2cooh) M = 75mentioning

confidence: 95%

“…The presence of water has long been established for IRAS 16293-2422. It was first observed thanks to masers (Wilking & Claussen 1987), which were quickly realized to be associated with source A (Wootten 1989;Alves et al 2012) and to also be rapidly variable (Imai, Iwata & Miyoshi 1999;Colom et al 2016). H2O and HDO emission has since been detected at radio frequencies on envelope scales (van Dishoeck et al 1995;Stark et al 2004;Caux et al 2011;Lis et al 2016), and has been claimed to originate from both sources, A and B (Chandler et al 2005;Parise et al 2005;Jørgensen et al 2011).…”

Section: Appendix C: Molecules Of Iras 16293-2422mentioning

confidence: 99%

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Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Drozdovskaya

Dishoeck

Rubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

131

102

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Our modern day Solar System has 4.6 × 10 9 yrs of evolution behind it with just a few relics of its birth conditions remaining. Comets are thought to be some of the most pristine tracers of the initial ingredients that were combined to produce the Earth and the other planets. Other low-mass protostars may be analogous to our proto-Sun and hence, could be used to study the building blocks necessary to form Solar-like systems. This study tests this idea on the basis of new high sensitivity, high spatial resolution ALMA data on the protoplanetary discscales (∼ 70 au) of IRAS 16293-2422 and the bulk composition of comet 67P/Churyumov-Gerasimenko, as determined for the first time with the unique in situ monitoring carried out by Rosetta. The comparative analysis of the observations from the Protostellar Interferometric Line Survey (PILS) and the measurements made with Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) shows that the relative abundances of CHO-, N-, and Sbearing molecules correlate, with some scatter, between protostellar and cometary data. A tentative correlation is seen for the first time for P-and Cl-bearing compounds. The results imply that the volatile composition of cometesimals and planetesimals is partially inherited from the pre-and protostellar phases of evolution.

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“…OD has also been discovered on these scales with SOFIA (Parise et al 2012). OH has been observed at cm wavelengths and its emission appears to have variable flares (Colom et al 2016).…”

Section: C123 Glycine (Nh2ch2cooh) M = 75mentioning

confidence: 95%

Section: Appendix C: Molecules Of Iras 16293-2422mentioning

confidence: 99%

Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Drozdovskaya

Dishoeck

Rubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

131

102

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“…[16]). Single-dish monitoring of maser emission in the source suggests that the H 2 O maser flares are most probably linked to motions of shocked gas [14]. Our analysis of the VLBI data available in literature indicates that H 2 O masers in IRAS 16293 could trace shocks excited by a precessing outflow system (see Fig.…”

Section: Pos(evn2021)021mentioning

confidence: 69%

“…The source A2 shows highly variable, but bright 22 GHz H 2 O maser with the flux density of tens of kJy during flares and no less than 100 Jy in a stable state [14]. The flaring features appear alternately at blueshifted and redshifted velocities with respect to the cloud velocity of ∼4 km s −1 , typically in the velocity range of −5 -10 km s −1 .…”

Section: Iras 16293-2422mentioning

confidence: 97%

“…Note that observation of [18] was made during a quiescent state of the maser and blueshifted features were not detected. Monitoring of [14] indicated that the activity of the H 2 O maser in IRAS 16293 has a cyclic character, and the period of 2006-2008 was one of the longest maser emission minima. Thus, it is possible that the shocks traced by the H2O maser and presented in [15,16] and [17] no longer exist, and with VLBI observation of the maser emission associated with the new flare, we can catch the launch of young ejection bow shocks.…”

Section: Pos(evn2021)021mentioning

confidence: 99%

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Episodic ejection from a low-mass young stellar object traced by H2O masers

Szabó¹,

Bayandina²,

Kóspál³

et al. 2022

Proceedings of European VLBI Network Mini-Symposium and Users' Meeting 2021 — PoS(EVN2021)

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We present the project of a VLBI study of the 22 GHz H 2 O maser in a prototypical low-mass protostellar system IRAS 16293-2422. The observation was conducted to characterise the cause of the newly discovered enhanced maser activity in the source and to study the source's ejection behaviour as traced by maser emission. Single-dish monitoring and analysis of archival data indicate that the activity of the H 2 O maser in IRAS 16293-2422 has a cyclic character and traces episodic ejection events in the source. A new maser flare was recently discovered in a spectral feature that has never shown such a significant increase in flux density before. The flare of this feature seems to indicate the beginning of a new cycle of activity.

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Evolution of superflares of H2O maser emission in IRAS 16293–2422

Colom

Ashimbaeva

Lekht

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The aim of this work was to continue the monitoring of the H2O maser emission in IRAS 16293–2422 to detect superflares. We have been observing H2O maser emission at a wavelength of 1.35 cm towards the source IRAS 16293–2422 since 1999. The observations have been carried out with the 22-m radio telescope of the Pushchino Radio Astronomy Observatory (Russia). In 2007–2018, we also conducted several sessions of observations in OH lines at a wavelength of 18 cm in both circular polarizations with the Nançay Radio Telescope (France). Between 1997 and 2021, we observed three cycles of high activity of the H2O maser with a period of 8 yr. This variability could be related to the changing activity of the protostar in the tight binary system of IRAS 16293–2422 in the process of its formation. This variability could be related to an increase in the activity of the tight binary protostar IRAS 16293–2422 A, first seen in 2002. The H2O maser variation in flux density and radial velocity suggests that disturbances are propagating through organized structures in the form of chains ∼3.5 au long, with monotonic velocity gradients in the direction of propagation. The 18-cm OH emission in the main and satellite lines is thermal.

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Long-term monitoring and interpretation of flares in the H2O maser emission of IRAS 16293–2422

Cited by 7 publications

References 22 publications

Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Episodic ejection from a low-mass young stellar object traced by H2O masers

Evolution of superflares of H2O maser emission in IRAS 16293–2422

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