<i>Planck</i>intermediate results. XVIII. The millimetre and sub-millimetre emission from planetary nebulae

Arnaud, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Buemi, C. S.; Burigana, C.; Cardoso, J.-F.; Casassus, S.; Catalano, A.; Cerrigone, L.; Chamballu, A.; Chiang, H. C.; Colombi, S.; Colombo, L. P. L.; Couchot, F.; Crill, B. P.; Curto, A.; Cuttaia, F.; Davies, R. D.; Davis, R. J.; Bernardis, P. de; Rosa, A. de; Zotti, G. de; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Donzelli, S.; Doré, O.; Dupac, X.; Enßlin, T. A.; Eriksen, H. K.; Finelli⋆, F.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; González‐Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D. L.; Hildebrandt, S. R.; Hivon, E.; Holmes, W. A.; Hora, J. L.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lähteenmäki, A.; Lamarre, J.-M.; Lasenby, A.; Lawrence, C. R.; Leonardi, R.; Leto, P.; Lilje, P. B.; Linden-Vørnle, M.; López‐Caniego, M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Martín, P. G.; Masi, S.; Massardi, M.; Matarrese, S.; Mazzotta, P.; Mendes, L.; Mennella, A.; Migliaccio, M.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, John A.; Naselsky, P.; Nati, F.; Natoli, P.; Noviello, F.; Novikov, D.; Новиков, И. Д.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Peel, M.; Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, É.; Polenta, G.; Popa, L.; Pratt, G. W.; Procopio, P.; Prunet, S.; Puget, J.‐L.; Rachen, J. P.; Reinecke, M.; Remazeilles, M.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Trigilio, C.; Tristram, M.; Trombetti, T.; Tucci, M.; Umana, G.; Väliviita, J.; Tent, B. Van; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Zacchei, A.; Zijlstra, A. A.; Zonca, A.

doi:10.1051/0004-6361/201423836

Cited by 14 publications

(2 citation statements)

References 152 publications

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“…8-8 M ). [24][25][26][27] Until recently there have only been a handful of laboratory experiments potentially relevant to photoionization fronts. Most have made use of carbon foams or low-density plastics illuminated by x-ray sources.…”

Section: Introductionmentioning

confidence: 99%

“…23 Photoionization fronts are also important in the transition between "pre-planetary" to "planetary" nebula during the late-stage evolution of intermediate mass stars (∼0.8-8 M ). [24][25][26][27] Until recently there have only been a handful of laboratory experiments potentially relevant to photoionization fronts. Most have made use of carbon foams or low-density plastics illuminated by x-ray sources.…”

Section: Introductionmentioning

confidence: 99%

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Atomic modeling of photoionization fronts in nitrogen gas

et al. 2019

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Photoionization fronts play a dominant role in many astrophysical environments, but remain difficult to achieve in a laboratory experiment. Recent papers have suggested that experiments using a nitrogen medium held at ten atmospheres of pressure that is irradiated by a source with a radiation temperature of T R ∼ 100 eV can produce viable photoionization fronts. We present a suite of one-dimensional numerical simulations using the Helios multi-material radiation hydrodynamics code that models these conditions and the formation of a photoionization front. We study the effects of varying the atomic kinetics and radiative transfer model on the hydrodynamics and ionization state of the nitrogen gas, finding that more sophisticated physics, in particular a multi-angle long characteristic radiative transfer model and a collisional-radiative atomics model, dramatically changes the atomic kinetic evolution of the gas. A photoionization front is identified by computing the ratios between the photoionization rate, the electron impact ionization rate, and the total recombination rate. We find that due to the increased electron temperatures found using more advanced physics that photoionization fronts are likely to form in our nominal model. We report results of several parameter studies. In one of these, the nitrogen pressure is fixed at ten atmospheres and varies the source radiation temperature while another fixes the temperature at 100 eV and varied the nitrogen pressure. Lower nitrogen pressures increase the likelihood of generating a photoionization front while varying the peak source temperature has little effect.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Atomic modeling of photoionization fronts in nitrogen gas

et al. 2019

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The State-of-Play of Anomalous Microwave Emission (AME) research

Dickinson

Ali-Haı̈moud

Barr

et al. 2018

New Astronomy Reviews

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Anomalous Microwave Emission (AME) is a component of diffuse Galactic radiation observed at frequencies in the range ≈ 10-60 GHz. AME was first detected in 1996 and recognised as an additional component of emission in 1997. Since then, AME has been observed by a range of experiments and in a variety of environments. AME is spatially correlated with far-IR thermal dust emission but cannot be explained by synchrotron or free-free emission mechanisms, and is far in excess of the emission contributed by thermal dust emission with the power-law opacity consistent with the observed emission at sub-mm wavelengths. Polarization observations have shown that AME is very weakly polarized ( 1 %). The most natural explanation for AME is rotational emission from ultra-small dust grains ("spinning dust"), first postulated in 1957.

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Herschelimaging of the dust in the Helix nebula (NGC 7293)

Steene

Hoof

Exter

et al. 2015

A&A

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Aims. In our series of papers presenting the Herschel imaging of evolved planetary nebulae, we present images of the dust distribution in the Helix nebula (NGC 7293). Methods. Images at 70, 160, 250, 350, and 500 µm were obtained with the PACS and SPIRE instruments on board the Herschel satellite.Results. The broadband maps show the dust distribution over the main Helix nebula to be clumpy and predominantly present in the barrel wall. We determined the spectral energy distribution of the main nebula in a consistent way using Herschel, IRAS, and Planck flux values. The emissivity index of β = 0.99 ± 0.09, in combination with the carbon rich molecular chemistry of the nebula, indicates that the dust consists mainly of amorphous carbon. The dust excess emission from the central star disk is detected at 70 µm and the flux measurement agrees with previous measurement. We present the temperature and dust column density maps. The total dust mass across the Helix nebula (without its halo) is determined to be 3.5 × 10 −3 M at a distance of 216 pc. The temperature map shows dust temperatures between 22 K and 42 K, which is similar to the kinetic temperature of the molecular gas, confirming that the dust and gas co-exist in high density clumps. Archived images are used to compare the location of the dust emission in the far infrared (Herschel) with the ionized (GALEX and Hβ) and molecular (H 2 ) component. The different emission components are consistent with the Helix consisting of a thick walled barrel-like structure inclined to the line of sight. The radiation field decreases rapidly through the barrel wall.

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Planckintermediate results. XVIII. The millimetre and sub-millimetre emission from planetary nebulae

Cited by 14 publications

References 152 publications

Atomic modeling of photoionization fronts in nitrogen gas

Atomic modeling of photoionization fronts in nitrogen gas

The State-of-Play of Anomalous Microwave Emission (AME) research

Herschelimaging of the dust in the Helix nebula (NGC 7293)

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