TY  - JOUR
A1  - Rubio, Gabriel
A1  - Toalá, Jesús Alberto
A1  - Todt, Helge Tobias
A1  - Sabin, Laurence
A1  - Santamaría, Edgar
A1  - Ramos-Larios, Gerardo
A1  - Martín Guerrero, José David
T1  - Planetary nebulae with Wolf-Rayet-type central stars - IV. NGC 1501 and its mixing layer
T2  - Monthly notices of the Royal Astronomical Society
N2  - Theory predicts that the temperature of the X-ray-emitting gas (similar to 10(6) K) detected from planetary nebulae (PNe) is a consequence of mixing or thermal conduction when in contact with the ionized outer rim (similar to 10(4) K). Gas at intermediate temperatures (similar to 10(5) K) can be used to study the physics of the production of X-ray-emitting gas, via C iv, N v, and O vi ions. Here, we model the stellar atmosphere of the CSPN of NGC 1501 to demonstrate that even this hot H-deficient [WO4]-type star cannot produce these emission lines by photoionization. We use the detection of the C iv lines to assess the physical properties of the mixing region in this PNe in comparison with its X-ray-emitting gas, rendering NGC 1501 only the second PNe with such characterization. We extend our predictions to the hottest [WO1] and cooler [WC5] spectral types and demonstrate that most energetic photons are absorbed in the dense winds of [WR] CSPN and highly ionized species can be used to study the physics behind the production of hot bubbles in PNe. We found that the UV observations of NGC 2452, NGC 6751, and NGC 6905 are consistent with the presence mixing layers and hot bubbles, providing excellent candidates for future X-ray observations.
KW  - stars: evolution
KW  - stars: individual: WD0402+607
KW  - stars: winds
KW  - outflows;
KW  - stars: Wolf-Rayet
KW  - planetary nebulae: general
KW  - planetary nebulae
KW  - individual: NGC1501
Y1  - 2022
UR  - https://publishup.uni-potsdam.de/frontdoor/index/index/docId/61218
SN  - 0035-8711
SN  - 1365-2966
VL  - 517
IS  - 4
SP  - 5166
EP  - 5179
PB  - Oxford Univ. Press
CY  - Oxford
ER  -