HST STIS UV Spectroscopic Observations of the Protoplanetary Nebula Hen3-1475<sup>∗</sup>
                  <sup>†</sup>

Fang, Xuan; Castro, Ana Inés Gómez de; Toalá, J. A.; Riera, A.

doi:10.3847/2041-8213/aae20c

Cited by 5 publications

(4 citation statements)

References 25 publications

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“…The actual jet dynamics within the lobes could be more complex than previously anticipated. An investigation of the multi-epoch HST F658N images suggests that the outer knots (NW2/SE2 and NW3/SE3) of Hen 3-1475 may not be the radially fast-moving "bullets" as previously thought, but locally excited due to Kelvin-Helmholtz instabilities [14]. If this is true, then NW2/SE2 and NW3/SE3 are probably different from NW1/SE1 in terms of formation and excitation.…”

Section: Jet Kinematics and Preliminary Interpretationmentioning

confidence: 89%

UV Monochromatic Imaging of the Protoplanetary Nebula Hen 3-1475 Using HST STIS

et al. 2018

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Collimated outflows and jets play a critical role in shaping planetary nebulae (PNe), especially in the brief transition from a spherical AGB envelope to an aspherical PN, which is called the protoplanetary nebula (pPN) phase. We present UV observations of Hen 3-1475, a bipolar pPN with fast, highly collimated jets, obtained with STIS on board the Hubble Space Telescope (HST). The deep, low-dispersion spectroscopy enabled monochromatic imaging of Hen 3-1475 in different UV nebular emission lines; this is the first of such attempt ever conducted for a pPN. The northwest inner knot (NW1) is resolved into four components in Mg ii λ 2800. Through comparison analysis with the HST optical narrowband images obtained 6 yr earlier, we found that these components of NW1 hardly move, despite of a negative gradient of high radial velocities, from −1550 km s - 1 on the innermost component to ∼−300 km s - 1 on the outermost. These NW1 knot components might thus be quasi-stationary shocks near the tip of the conical outflow of Hen 3-1475.

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Section: Jet Kinematics and Preliminary Interpretationmentioning

confidence: 89%

UV Monochromatic Imaging of the Protoplanetary Nebula Hen 3-1475 Using HST STIS

et al. 2018

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“…The selfabsorption of X-rays by gas within the nebula considerably reduces the detection of soft X-rays, and this provides a plausible explanation for the lack of detection of X-ray emission in the other parts of the nebula, given the sensitivity of Chandra. Finally, the emission of [NII] and [SII] in Hen 3-1475 (see Fang et al 2018 and references therein) is related to shocked gas of moderate temperatures, and it is likely that they arise from the jets and the forward shock of the bipolar nebula. However, the jets in Hen 3-1475 are broken into bullets of gas, which are a natural consequence of neck instabilities (Jackson 1962).…”

Section: Discussionmentioning

confidence: 99%

“…This article also investigates the self-magnetic collimation of the winds, and we are able to reproduce in general terms two observed objects, HD 101584 (Olofsson et al 2019) observed with the Atacama Large Millimeter Array (ALMA) and Hen 3-1475 (Fang et al 2018) observed with the Hubble Space Telescope (HST), in which the process of self-collimation can be directly observed.…”

Section: Introductionmentioning

confidence: 99%

Common Envelope Shaping of Planetary Nebulae. II. Magnetic Solutions and Self-collimated Outflows

Garcı́a-Segura

Taam

Ricker

2020

ApJ

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Magnetic fields of order 10 1 −10 2 gauss that are present in the envelopes of red giant stars are ejected in common envelope scenarios. These fields could be responsible for the launching of magnetically driven winds in proto-planetary nebulae. Using 2D simulations of magnetized winds interacting with an envelope drawn from a 3D simulation of the common envelope phase, we study the confinement, heating, and magnetic field development of post-common envelope winds. We find that the ejected magnetic field can be enhanced via compression by factors up to ∼ 10 4 in circumbinary disks during the self-regulated phases. We find values for the kinetic energy of the order of 10 46 erg that explain the large values inferred in proto-planetary nebula outflows. We show that the interaction of the formed circumbinary disk with a spherical, stellar wind produces a "tapered" flow that is almost indistinguishable from an imposed tapered flow. This increases the uncertainty of the origin of protoplanetary nebula winds, which could be either stellar, circumstellar (stellar accretion disk), circumbinary (circumbinary accretion disk), or a combination of all three.Within this framework, a scenario for self-collimation of weakly magnetized winds is discussed, which can explain the two objects where the collimation process is observationally resolved, HD 101584 and Hen 3-1475. An explanation for the equatorial, molecular hydrogen emission in CRL 2688 is also presented.

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“…The transformation lasts a few thousand years at most and the PPN is largely obscured until a combination of expansion and dust expulsion brings it into view. In this time, a usually quite spherical shape of the post-AGB envelope may distort into a dynamic display of winds, bullets and jets, creating rings, ellipses, butterflies and funnels, as summarised by Fang et al (2018b). Highresolution images investigated by Corradi & Schwarz (1995) show ∼ 64% of outflows arrive at the PN stage as elliptical.…”

Section: Introductionmentioning

confidence: 99%

Numerical simulations of wind-driven protoplanetary nebulae. II. signatures of atomic emission

Новиков

Smith

2019

Monthly Notices of the Royal Astronomical Society

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We follow up on our systematic study of axisymmetric hydrodynamic simulations of protoplanetary nebula. The aim of this work is to generate the atomic analogues of the H 2 near-infrared models of Paper I with the ZEUS code modified to include molecular and atomic cooling routines. We investigate stages associated with strong [Fe II] 1.64 µm and [S II] 6716Å forbidden lines, the [O I] 6300Å airglow line, and Hα 6563Å emission. We simulate (80 ∼ 200 km s −1 ) dense (∼ 10 5 cm −3 ) outflows expanding into a stationary ambient medium. In the case of an atomic wind interacting with an atomic medium, a decelerating advancing turbulent shell thickens with time. This contrasts with all other cases where a shell fragments into a multitude of cometary-shaped protrusions with weak oblique shocks as the main source of gas excitation. We find that the atomic wind-ambient simulation leads to considerably higher excitation, stronger peak and integrated atomic emission as the nebula expands. The weaker emission when one component is molecular is due to the shell fragmentation into fingers so that the shock surface area is increased and oblique shocks are prevalent. Position-velocity diagrams indicate that the atomic-wind model may be most easy to distinguish with more emission at higher radial velocities. With post-AGB winds and shells often highly obscured and the multitude of configurations that are observed, this study suggests and motivates selection criteria for new surveys.

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HST STIS UV Spectroscopic Observations of the Protoplanetary Nebula Hen3-1475^∗ ^†

Abstract: We present UV spectra of the protoplanetary nebula (pPN) Hen 3-1475 obtained with the Space

Cited by 5 publications

References 25 publications

UV Monochromatic Imaging of the Protoplanetary Nebula Hen 3-1475 Using HST STIS

UV Monochromatic Imaging of the Protoplanetary Nebula Hen 3-1475 Using HST STIS

Common Envelope Shaping of Planetary Nebulae. II. Magnetic Solutions and Self-collimated Outflows

Numerical simulations of wind-driven protoplanetary nebulae. II. signatures of atomic emission

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HST STIS UV Spectroscopic Observations of the Protoplanetary Nebula Hen3-1475∗ †

Abstract: We present UV spectra of the protoplanetary nebula (pPN) Hen 3-1475 obtained with the Space

Cited by 5 publications

References 25 publications

UV Monochromatic Imaging of the Protoplanetary Nebula Hen 3-1475 Using HST STIS

UV Monochromatic Imaging of the Protoplanetary Nebula Hen 3-1475 Using HST STIS

Common Envelope Shaping of Planetary Nebulae. II. Magnetic Solutions and Self-collimated Outflows

Numerical simulations of wind-driven protoplanetary nebulae. II. signatures of atomic emission

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HST STIS UV Spectroscopic Observations of the Protoplanetary Nebula Hen3-1475^∗ ^†