Photodissociation in proto-planetary nebulae

Garcı́a-Segura, Guillermo

doi:10.1051/0004-6361/201015585

Cited by 11 publications

(7 citation statements)

References 45 publications

(49 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The true 3D dynamical structure of PNe has been a problem of great complexity for many years. According to theoretical research, the deviation of PNe structure from spherical symmetry occurs for several reasons: (i) the presence of strong magnetic fields and/or the rotation of the central star (García‐Segura 1997; García‐Segura et al 1999); (ii) the effect of photodissociation (García‐Segura 2010) and (iii) the binarity of central stars (Balick & Frank 2002). Morphological and kinematical studies of PNe help to understand their formation and evolution processes.…”

Section: Introductionmentioning

confidence: 99%

‘Distance mapping’ and the 3D structure of BD +30° 3639

Akras¹,

Steffen²

2012

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

BD +30 • 3639 is a member of a group of uncommon planetary nebulae with Wolf-Rayet central star and higher expansion velocities in [O III] than in [N II] lines. Images and highresolution spectra from the literature are used in order to construct a 3D model of the nebula using the morpho-kinematic code SHAPE. We find that two homologous expansion laws are needed for the [N II] and [O III] shells. We conclude that the internal velocity field of BD +30 • 3639 decreases with the distance from the central star at least between the [O III] and [N II] shells. A cylindrical velocity component is used to replicate the high-speed bipolar collimated outflows. We also present a new kinematic analysis technique called 'distance mapping'. It uses the observed proper motion vectors and the 3D velocity field to generate maps that can be used as a constraint to the morpho-kinematic modelling with SHAPE as well as improve the accuracy for distance determination. It is applied to BD +30 • 3639 using 178 internal proper motion vectors from Li, Harrington & Borkowski and our 3D velocity field to determine a distance of 1.52 ± 0.21 kpc. Finally, we find evidence for an interaction between the eastern part of the nebula and the ambient H 2 molecular gas.

show abstract

Section: Introductionmentioning

confidence: 99%

‘Distance mapping’ and the 3D structure of BD +30° 3639

Akras¹,

Steffen²

2012

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Figure 2. Cuts through the density distribution of hydrodynamical simulations of the multi-polar structure formations through instabilities in photo-dissociation regions is shown (García-Segura, 2011) In the past it has been rare to see hydrodynamical simulations that were tailored for a particular object. With progress in numerical computing capabilities, this is more viable now.…”

Section: Jets and Bulletsmentioning

confidence: 99%

Dynamical modeling and the interactions with the ISM

Steffen¹

2011

Proc. IAU

View full text Add to dashboard Cite

Abstract. This paper is a review of some of the recent modeling efforts to improve our understanding of structure formation and evolution of planetary nebulae including their interaction with the interstellar medium. New propositions have been made for the formation mechanism of multi-polar PNe and PPNe. These mechanisms are based on the central engine with interacting binary stars or hole producing instabilities in expanding shock waves leading to illumination effects from the central star that change the appearance of the nebula. Furthermore, there has been a lot of progress in the observation and 3D modeling of the kinematics, which is key to the understanding of the dynamics. Extensive observational catalogs are coming online for the kinematics, as well as some very detailed proper motion measurements have been made. New techniques for morpho-kinematic 3D modeling help to make the interpretation of kinematic data more reliable and detailed. In addition to individual pointed observations, new surveys have lead to the discovery of many PNe that show clear signs of interaction with the interstellar medium. Systematic hydrodynamic models of the interaction have produced a general scheme for the observed structure that results from the interaction of an evolving planetary nebula with the ISM. Detailed modeling of the dust-gas dynamics during the interaction with the ISM have produced interesting predictions for future IR observations. Detailed models were worked out for the structure of the bowshock and tail of Mira that was recently discovered in the UV.

show abstract

“…Thus, the number of observable early-type stars are highly limited compared with that of later types. Besides, early-type stars are famous for their strong stellar wind to produce considerable circumstellar material (Garcia-Segura et al 1996), which brings about uncertainty in determining their stellar properties. Consequently, their intrinsic colors are not well determined.…”

Section: Introductionmentioning

confidence: 99%

Intrinsic Color Indices of Early-type Dwarf Stars

Deng

Sun

Jian

et al. 2020

View full text Add to dashboard Cite

Early-type stars are short lived and scarce in comparison with other types. Based on the recently released catalogs of early type stars from the largest LAMOST spectroscopic survey, the intrinsic colors of the stars with effective temperature up to 32,000 K are determined for the bands from ultraviolet to infrared by using the blue-edge method. Analytic relations are derived for the intrinsic color index with the effective temperature for the WISE, 2MASS, Gaia, APASS, SDSS, Pan-STARRS1, and GALEX bands. The results are generally consistent with previous works. In addition, the intrinsic colors of O-type dwarfs and OB supergiants are roughly estimated.

show abstract

Photodissociation in proto-planetary nebulae

Cited by 11 publications

References 45 publications

‘Distance mapping’ and the 3D structure of BD +30° 3639

‘Distance mapping’ and the 3D structure of BD +30° 3639

Dynamical modeling and the interactions with the ISM

Intrinsic Color Indices of Early-type Dwarf Stars

Contact Info

Product

Resources

About