Multiwavelength observations of NaSt1 (WR 122): equatorial mass loss and X-rays from an interacting Wolf–Rayet binary

Mauerhan, Jon C.; Smith, Nathan; Dyk, Schuyler D. Van; Morzinski, Katie M.; Close, Laird M.; Hinz, Philip M.; Males, Jared R.; Rodigas, Timothy J.

doi:10.1093/mnras/stv257

Cited by 16 publications

(27 citation statements)

References 56 publications

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“…In the thermal infrared, the system is adorned with a prominent ≈ 12 ′′ spiral dust plume, revealed by proper motion studies to be expanding at only ≈ 570 km s −1 . As the dust and gas appear coeval, these observations are inconsistent with existing models of the dynamics of such colliding wind systems 5,6,7 . We propose that this contradiction can be resolved if the system is capable of launching extremely anisotropic winds.…”

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confidence: 65%

Anisotropic winds in a Wolf–Rayet binary identify a potential gamma-ray burst progenitor

et al. 2018

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INTRODUCTORY PARAGRAPHThe massive evolved Wolf-Rayet stars sometimes occur in colliding-wind binary systems in which dust plumes are formed as a result of the collision of stellar winds 1 . These structures are known to encode the parameters of the binary orbit and winds 2,3,4 . Here, we report observations of a previously undiscovered Wolf-Rayet system, 2XMM J160050.7-514245, with a spectroscopically determined wind speed of ≈ 3400 km s −1 . In the thermal infrared, the system is adorned with a prominent ≈ 12 ′′ spiral dust plume, revealed by proper motion studies to be expanding at only ≈ 570 km s −1 . As the dust and gas appear coeval, these observations are inconsistent with existing models of the dynamics of such colliding wind systems 5,6,7 . We propose that this contradiction can be resolved if the system is capable of launching extremely anisotropic winds. Near-critical stellar rotation is known to drive such winds 8,9 , suggesting this Wolf-Rayet system as a potential Galactic progenitor system for long-duration gamma-ray bursts.Corresponding author: J. R. Callingham callingham@astron.nl 2 CALLINGHAM ET AL. MAIN BODYWolf-Rayet (WR) stars represent the final stage of the evolution of the most massive stars before ending their lives as supernovae. Late-type carbon-rich WR stars with binary companions have the potential to produce spiral "Pinwheel" patterns in which dust forms at the interface between the colliding stellar winds 2,10 . As the orbital motion entangles the winds, the form of the plume encodes the primary wind and orbital parameters, forming rare and powerful laboratories for testing our understanding of the mass-loss in WR stars. For well studied Pinwheels such as WR 104 2,4 , WR 98a 3 and WR 140 11,12 , nearly complete solutions can be obtained that tightly constrain the wind speeds, wind-momentum ratio, and orbital parameters. For WR 104 and WR 140, the dust (studied by its proper motion in the thermal infrared) and the gas (the dominant wind component in the line of sight revealed by spectroscopy) have been shown to be co-moving, as expected for spherical stellar winds.Additionally, WR stars play a significant role in the chemistry and kinetic energy budget of the interstellar medium 1 , and are considered to be likely progenitors to long-duration gamma-ray bursts (GRBs) 13,14 . A key ingredient in most models for the production of long-duration GRBs is rapid rotation of the WR progenitor star 13 . For stars that have solar-like metallicity, as observed for most Galactic WR stars 15,16 , line-driven winds rapidly rob the star of angular momentum. One channel to produce near critical-rotation of the WR star before undergoing a core-collapse supernova is through binary interaction 17 . Unfortunately debates over the role of rotation remain largely in the domain of theory as it has proven extremely difficult to place any observational constraints on the rotation of WR stars. Because WR spectra are generally formed in their extended dense winds 18 , obtaining rotational velocity from fitting t...

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confidence: 65%

Anisotropic winds in a Wolf–Rayet binary identify a potential gamma-ray burst progenitor

et al. 2018

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“…Such an event is thought to produce stripped-envelope WRs and is claimed to be occurring ininteracting binary systems, such as NaSt1 (e.g., Crowther & Smith 1999;Mauerhan et al 2015) and RY Scuti (Smith et al 2011). Both systems host a WR-like star surrounded by a dusty, hydrogen-rich shell and may therefore be an example of a possible SN 2014C progenitor.…”

Section: Sn 2014c: An Interacting Stripped-envelope Supernova With a mentioning

confidence: 99%

A Systematic Study of Mid-Infrared Emission From Core-Collapse Supernovae With Spirits

Tinyanont

Kasliwal

Fox

et al. 2016

ApJ

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We present a systematic study of mid-infrared emission from 141 nearby supernovae (SNe)observed with Spitzer/ IRAC as part of the ongoing SPIRITS survey. We detect 8 Type Ia and 36 core-collapse SNe. All TypeIa/Ibc SNebecome undetectable within threeyears of explosion, whereas 22±11% of TypeII SNecontinue to be detected. Five TypeII SNe are detected even two decades after discovery (SN 1974E, 1979C, 1980K, 1986J, and 1993J). Warm dust luminosity, temperature, and a lower limit on mass are obtained by fitting the two IRAC bands, assuming an optically thin dust shell. We derive warm dust masses between 10 −6 and 10 −2 M e and dust color temperatures between 200 and 1280 K. This observed warm dust could be pre-existing or newly created, but in either case represents a lower limit to the dust mass because cooler dust may be present. We present three case studies of extreme SNe.SN 2011ja (II-P) was over-luminous ([4.5] = −15.6 mag) at 900 days post explosion with increasing hot dust mass, suggesting either an episode of dust formation or intensifying circumstellar material (CSM) interactions heating up pre-existing dust. SN 2014bi (II-P) showed a factor of 10 decrease in dust mass over one month, suggesting either dust destruction or reduced dust heating. The IR luminosity of SN 2014C (Ib) stayedconstant over 800 days, possibly due to strong CSM interaction with anH-rich shell, which is rare among stripped-envelope SNe. The observations suggest that this CSM shell originated from an LBV-like eruption roughly 100 years pre-explosion. The observed diversity demonstrates the power of mid-IR observations of a large sample of SNe.

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“…One possible explanation for the rapid evolution of WR112 may be mass transfer via interactions with a close binary companion (e.g., Smith et al 2011a). Two notable examples of observed mass transfer likely leading to a stripped-envelope WR star are NaSt1 (Mauerhan et al 2015) and RY Scuti (Smith et al 2011b). WR112 may therefore be another such example of binary interaction influencing the evolution of massive stars.…”

Section: On the Nature Of The Wr112 Nebula: Mass Loss From A Previoumentioning

confidence: 99%

Stagnant Shells in the Vicinity of the Dusty Wolf–Rayet–OB Binary WR 112

Lau

Hankins

Schödel

et al. 2017

ApJL

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We present high spatial resolution mid-infrared images of the nebula around the late-type carbon-rich Wolf-Rayet (WC)-OB binary system WR112 taken by the recently upgraded VLT spectrometer and imager for the midinfrared (VISIR) with the PAH1, Ne II_2, and Q3 filters. The observations reveal a morphology resembling a series of arc-like filaments and broken shells. Dust temperatures and masses are derived for each of the identified filamentary structures, which exhibit temperatures ranging from -+ 179 6 8 K at the exterior W2 filament to -+ 355 25 37 K in the central 3″. The total dust mass summed over the features is 2.6±0.4×10−5 M e . A multi-epoch analysis of mid-IR photometry of WR112 over the past ∼20 years reveals no significant variability in the observed dust temperature and mass. The morphology of the mid-IR dust emission from WR112 also exhibits no significant expansion from imaging data taken in 2001, 2007, and 2016, which disputes the current interpretation of the nebula as a high expansion velocity (∼1200 km s −1 ) "pinwheel"-shaped outflow driven by the central WC-OB collidingwind binary. An upper limit of 120 km s −1 is derived for the expansion velocity assuming a distance of 4.15kpc. The upper limit on the average total mass-loss rate from the central 3″ of WR112 is estimated to be. We leave its true nature as an open question, but propose that the WR112 nebula may have formed in the outflow during a previous red or yellow supergiant phase of the central Wolf-Rayet star.

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Multiwavelength observations of NaSt1 (WR 122): equatorial mass loss and X-rays from an interacting Wolf–Rayet binary

Cited by 16 publications

References 56 publications

Anisotropic winds in a Wolf–Rayet binary identify a potential gamma-ray burst progenitor

Anisotropic winds in a Wolf–Rayet binary identify a potential gamma-ray burst progenitor

A Systematic Study of Mid-Infrared Emission From Core-Collapse Supernovae With Spirits

Stagnant Shells in the Vicinity of the Dusty Wolf–Rayet–OB Binary WR 112

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