A Review of Telecine Systems

Morse, D. R.

doi:10.5594/j12071

Cited by 5 publications

(4 citation statements)

References 15 publications

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“…The physical conditions, chemistry, and location of these structures are therefore direct tracers of significant nonspherical mass loss events and stellar wind processes dur-pamorris@caltech.edu ing the evolution of the system. η Car is probably the most luminous star in the Milky Way (Davidson & Humphreys 1997;Groh et al 2012) and certainly one of the most energetic and best known examples of an evolved system that has undergone multiple high-mass eruptions, traced by its wellrecorded light curve variations (Smith & Frew 2011;Damineli et al 2019), and the formation of a circumstellar bipolar "Homunculus" nebula (Morse et al 2001) and massive structures in the equatorial plane. The equatorial structures, interpreted as a disrupted torus (Smith et al 2018a), were detected with mid-infrared imaging (Morris et al 1999;Polomski et al 1999), and harbor the bulk of the ≈0.25 M of dust , as well as a number of simple H-, C-, N-, and O-bearing molecules with upper level excitation energies to around 300 K (Loinard et al 2012(Loinard et al , 2016Morris et al 2017;Smith et al 2018a; Morris et al 2020;Gull et al 2020).…”

Section: Introductionmentioning

confidence: 99%

CO, Water, and Tentative Methanol in η Carinae Approaching Periastron

Morris

Charnley

Corcoran

et al. 2020

ApJL

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In circumstellar gas, the complex organic molecule methanol has been found almost exclusively around young stellar objects, and is thus regarded as a signpost of recent star formation. Here we report the first probable detection of methanol around an evolved high-mass star, in the complex circumstellar environment around the Luminous Blue Variable η Carinae, while using ALMA to investigate molecular cloud conditions traced by CO (2-1) in an orbit phase of the massive binary preceding the 2020 periastron. Favoring methanol over a 13 CS alternative, the emission originates from hot (T gas 700 K) material, ∼2 (0.02 pc) across, centered on the dust-obscured binary in contrast to the CO which traces inner layers of the extended massive equatorial torus, and is accompanied by prominent absorption in a cooler (T gas 110 K) layer of gas. We also report detections of water in Herschel/HIFI observations at 557 GHz and 988 GHz. The methanol abundance is several to 50 times higher than observed towards several lower mass stars, while water abundances are similar to those observed in cool, dense molecular clouds. The very high methanol:water abundance ratio in the core of η Carinae may suggest methanol formation processes similar to Fischer-Tropsch-type catalytic reactions on dust grains. These observations prove that complex molecule formation can occur in the chemically evolved environments around massive stars in the end stages of their evolution, given sufficient gas densities and shielding conditions as may occur in material around massive interacting companions and merger remnants.

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Section: Introductionmentioning

confidence: 99%

CO, Water, and Tentative Methanol in η Carinae Approaching Periastron

Morris

Charnley

Corcoran

et al. 2020

ApJL

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“…At least 10M , and potentially more than 40M , were ejected during this event (Morris et al 1999;Smith et al 2003a;Smith 2006;Gomez et al 2010), causing the formation of a dusty bipolar nebula known as the Homunculus (Gaviola 1950). Analysis of the proper motion of the Homunculus shows that the eruption happened in the 1840s (Currie et al 1996;Morse et al 2001). This, combined with its relative proximity (2.3 kpc, Allen & Hillier 1993;Smith 2006), means that the Homunculus's structure can be investigated in an unparalleled level of detail.…”

Section: Introductionmentioning

confidence: 99%

“…The interacting winds scenario requires a pre-existing slow and dense equatorial torus to pinch the waist of the bipolar structure. However, observations show that the thin equatorial disc or 'skirt' seen in optical images of the Homunculus is no older than the bipolar lobes and that there is not enough mass in the skirt to shape the overall morphology of the nebula Davidson et al 2001;Morse et al 2001;Smith 2006). The MHD model of Matt & Balick (2004) requires a huge field strength ( 2.5 × 10 4 G at the equator) to shape the large amount of mass ejected, and it is unclear if such a field was available.…”

Section: Introductionmentioning

confidence: 99%

The three-dimensional structure of the Eta Carinae Homunculus★

Steffen¹,

Teodoro

Madura

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We investigate, using the modeling code SHAPE, the three-dimensional structure of the bipolar Homunculus nebula surrounding Eta Carinae as mapped by new ESO VLT/X-Shooter observations of the H 2 λ = 2.12125µm emission line. Our results reveal for the first time important deviations from the axisymmetric bipolar morphology: 1) circumpolar trenches in each lobe positioned point-symmetrically from the center and 2) off-planar protrusions in the equatorial region from each lobe at longitudinal (∼ 55 • ) and latitudinal (10 • − 20 • ) distances from the projected apastron direction of the binary orbit. The angular distance between the protrusions (∼ 110 • ) is similar to the angular extent of each polar trench (∼ 130 • ) and nearly equal to the opening angle of the wind-wind collision cavity (∼ 110 • ). As in previous studies, we confirm a hole near the centre of each polar lobe and no detectable near-IR H 2 emission from the thin optical skirt seen prominently in visible imagery. We conclude that the interaction between the outflows and/or radiation from the central binary stars and their orientation in space has had, and possibly still has, a strong influence on the Homunculus. This implies that prevailing theoretical models of the Homunculus are incomplete as most assume a single star origin that produces an axisymmetric nebula. We discuss how the newly found features might be related to the Homunculus ejection, the central binary and the interacting stellar winds.

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“…prior to the SN explosion, where v CSM is the CSM ejection velocity. We note, for comparison, that the age of the η Car Homunculus Nebula is estimated to be about 1800 yr (Morse et al 2001;Smith et al 2017), and that Sarangi et al (2018) argued for the existstence of a cavity in SN 2010jl's CSM.…”

Section: Implications For Pre-explosion Mass-lossmentioning

confidence: 87%

A Six-year Image-subtraction Light Curve of SN 2010jl

Ofek

Zackay

Gal‐Yam

et al. 2019

PASP

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SN 2010jl was a luminous Type IIn supernova (SN), detected in radio, optical, X-ray and hard Xrays. Here we report on its six year R-and g-band light curves obtained using the Palomar Transient Factory. The light curve was generated using a pipeline based on the proper image subtraction method and we discuss the algorithm performances. As noted before, the R-band light curve, up to about 300 days after maximum light is well described by a power-law decline with a power-law index of α ≈ −0.5. Between day 300 and day 2300 after maximum light, it is consistent with a power-law decline, with a power-law index of about α ≈ −3.4. The longevity of the light curve suggests that the massive circum-stellar material around the progenitor was ejected on time scales of at least tens of years prior to the progenitor explosion.

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A Review of Telecine Systems

Cited by 5 publications

References 15 publications

CO, Water, and Tentative Methanol in η Carinae Approaching Periastron

CO, Water, and Tentative Methanol in η Carinae Approaching Periastron

The three-dimensional structure of the Eta Carinae Homunculus★

A Six-year Image-subtraction Light Curve of SN 2010jl

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