Hybrid polygon and hydrodynamic nebula modeling with multi-waveband radiation transfer in astrophysics

Steffen, W.; Koning, Nico

doi:10.1016/j.ascom.2017.06.002

Cited by 11 publications

(8 citation statements)

References 17 publications

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“…Each slit position indeed produces a position-velocity (PV) diagram that reveals the expansion of the nova remnants along the long-slit. This information will be used in conjunction with the direct images to investigate the 3D physical structure of the nova remnant using the morphokinematic modelling tool SHAPE 4 (version 5.0; Steffen & Koning 2017 ). This software allows constructing 3D model structures and producing synthetic images and PV maps under the assumption of homologous expansion that can be compared with the observed ones.…”

Section: R E S U Lt Smentioning

confidence: 99%

Spatiokinematic models of five nova remnants: correlations between nova shell axial ratio, expansion velocity, and speed class

Santamaría

Guerrero

Zavala

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present long-slit intermediate-dispersion spectroscopic observations and narrow-band direct imaging of four classical nova shells, namely T Aur, HR Del, DQ Her and QU Vul, and the nova-like source CK Vul. These are used to construct models of their nebular remnants using the morpho-kinematic modelling tool shape to reveal their 3D shape. All these nova remnants but CK Vul can be described by prolate ellipsoidal shells with different eccentricity degree, from the spherical QU Vul to the highly elongated shell with an equatorial component HR Del. On the other hand, CK Vul shows a more complex structure, with two pairs of nested bipolar lobes. The spatio-kinematic properties of the ellipsoidal nova shells derived from our models include their true axial ratios. This parameter is expected to correlate with the expansion velocity and decline time t3 (i.e. their speed class) of a nova as the result the interaction of the ejecta with the circumstellar material and rotation speed and magnetic field of the white dwarf. We have compared these three parameters including data available in the literature for another two nova shells, V533 Her and FH Ser. There is an anti-correlation between the expansion velocity and the axial ratio and decline time t3 for nova remnants with ellipsoidal morphology, and a correlation between their axial ratios and decline times t3, confirming theoretical expectations that the fastest expanding novae have the smallest axial ratios. We note that the high expansion velocity of the nova shell HR Del of 615 km s−1 is inconsistent with its long decline time t3 of 250 days.

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Section: R E S U Lt Smentioning

confidence: 99%

Spatiokinematic models of five nova remnants: correlations between nova shell axial ratio, expansion velocity, and speed class

Santamaría

Guerrero

Zavala

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Offset ( plane of the sky and counted positive from north towards the observer.) In an effort to test this interpretation, we constructed a 3dimensional model of the structure in Shape (Steffen et al 2010(Steffen et al , 2011Steffen & Koning 2017), including basic radiative transfer of CO utilizing the shapemol module (Santander-García et al 2015). The model was optimized by referring to the total intensity and channel maps, PV diagrams, and spectral profiles of the CO 3-2 emission.…”

Section: A 3-dimensional Model Of the Co Emittermentioning

confidence: 99%

Submillimeter-wave emission of three Galactic red novae: cool molecular outflows produced by stellar mergers

Kamiński

Steffen²,

Tylenda

et al. 2018

A&A

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Red novae are optical transients erupting at luminosities typically higher than those of classical novae. Their outbursts are believed to be caused by stellar mergers. We present millimeter/submillimeter-wave observations with ALMA and SMA of the three best known Galactic red novae, V4332 Sgr, V1309 Sco, and V838 Mon. The observations were taken 22, 8, and 14 yr after their respective eruptions and reveal the presence of molecular gas at excitation temperatures of 35-200 K. The gas displays molecular emission in rotational transitions with very broad lines (full width ∼400 km s −1 ). We found emission of CO, SiO, SO, SO 2 (in all three red novae), H 2 S (covered only in V838 Mon) and AlO (present in V4332 Sgr and V1309 Sco). No anomalies were found in the isotopic composition of the molecular material and the chemical (molecular) compositions of the three red novae appear similar to those of oxygen-rich envelopes of classical evolved stars (RSGs, AGBs, post-AGBs). The minimum masses of the molecular material that most likely was dispersed in the red-nova eruptions are 0.05, 0.01, and 10 −4 M for V838 Mon, V4332 Sgr, and V1309 Sco, respectively. The molecular outflows in V4332 Sgr and V1309 Sco are spatially resolved and appear bipolar. The kinematic distances to V1309 Sco and V4332 Sgr are 2.1 and 4.2 kpc, respectively. The kinetic energy stored in the ejecta of the two older red-nova remnants of V838 Mon and V4332 Sgr is of order 10 46 erg, similar to values found for some post-AGB (pre-PN) objects whose bipolar ejecta were also formed in a short-duration eruption. Our observations strengthen the link between these post-AGB objects and red novae and support the hypothesis that some of the post-AGB objects were formed in a common-envelope ejection event or its most catastrophic outcome, a merger.

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“…Each slit position indeed produces a position-velocity (PV) diagram that reveals the expansion of the nova remnants along the long-slit. This information will be used in conjunction with the direct images to investigate the 3D physical structure of the nova remnant using the morpho-kinematic modelling tool 4 (version 5.0; Steffen & Koning 2017). This software allows constructing 3D model structures and producing synthetic images and PV maps under the assumption of homologous expansion that can be compared with the observed ones.…”

Section: Resultsmentioning

confidence: 99%

Spatio-kinematic models of five nova remnants: correlations between nova shell axial ratio, expansion velocity, and speed class

Santamaría,

Guerrero,

Zavala

et al. 2022

Preprint

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We present long-slit intermediate-dispersion spectroscopic observations and narrow-band direct imaging of four classical nova shells, namely T Aur, HR Del, DQ Her and QU Vul, and the nova-like source CK Vul. These are used to construct models of their nebular remnants using the morpho-kinematic modelling tool to reveal their 3D shape. All these nova remnants but CK Vul can be described by prolate ellipsoidal shells with different eccentricity degree, from the spherical QU Vul to the highly elongated shell with an equatorial component HR Del. On the other hand, CK Vul shows a more complex structure, with two pairs of nested bipolar lobes. The spatio-kinematic properties of the ellipsoidal nova shells derived from our models include their true axial ratios. This parameter is expected to correlate with the expansion velocity and decline time 𝑡 3 (i.e., their speed class) of a nova as the result the interaction of the ejecta with the circumstellar material and rotation speed and magnetic field of the white dwarf. We have compared these three parameters including data available in the literature for another two nova shells, V533 Her and FH Ser. There is an anti-correlation between the expansion velocity and the axial ratio and decline time 𝑡 3 for nova remnants with ellipsoidal morphology, and a correlation between their axial ratios and decline times 𝑡 3 , confirming theoretical expectations that the fastest expanding novae have the smallest axial ratios. We note that the high expansion velocity of the nova shell HR Del of 615 km s −1 is inconsistent with its long decline time 𝑡 3 of 250 days.

show abstract

Hybrid polygon and hydrodynamic nebula modeling with multi-waveband radiation transfer in astrophysics

Cited by 11 publications

References 17 publications

Spatiokinematic models of five nova remnants: correlations between nova shell axial ratio, expansion velocity, and speed class

Spatiokinematic models of five nova remnants: correlations between nova shell axial ratio, expansion velocity, and speed class

Submillimeter-wave emission of three Galactic red novae: cool molecular outflows produced by stellar mergers

Spatio-kinematic models of five nova remnants: correlations between nova shell axial ratio, expansion velocity, and speed class

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