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Article: The chandra planetary nebula survey (chanplaNS). III. X-ray emission from the central stars of planetary nebulae

TitleThe chandra planetary nebula survey (chanplaNS). III. X-ray emission from the central stars of planetary nebulae
Authors
Keywordsplanetary nebulae
general
Issue Date2015
Citation
Astrophysical Journal Letters, 2015, v. 800, n. 1 How to Cite?
Abstract© 2015. The American Astronomical Society. All rights reserved. We present X-ray spectral analysis of 20 point-like X-ray sources detected in Chandra Planetary Nebula Survey observations of 59 planetary nebulae (PNe) in the solar neighborhood. Most of these 20 detections are associated with luminous central stars within relatively young, compact nebulae. The vast majority of these point-like X-ray-emitting sources at PN cores display relatively "hard" (≥0.5 keV) X-ray emission components that are unlikely to be due to photospheric emission from the hot central stars (CSPN). Instead, we demonstrate that these sources are well modeled by optically thin thermal plasmas. From the plasma properties, we identify two classes of CSPN X-ray emission: (1) high-temperature plasmas with X-ray luminosities, LX, that appear uncorrelated with the CSPN bolometric luminosity, L bol and (2) lower-temperature plasmas with L X/L bol 10-7. We suggest these two classes correspond to the physical processes of magnetically active binary companions and self-shocking stellar winds, respectively. In many cases this conclusion is supported by corroborative multiwavelength evidence for the wind and binary properties of the PN central stars. By thus honing in on the origins of X-ray emission from PN central stars, we enhance the ability of CSPN X-ray sources to constrain models of PN shaping that invoke wind interactions and binarity.
Persistent Identifierhttp://hdl.handle.net/10722/209045
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorMontez, Rodolfo-
dc.contributor.authorKastner, J. H.-
dc.contributor.authorBalick, Bruce-
dc.contributor.authorBehar, Ehud-
dc.contributor.authorBlackman, Eric G.-
dc.contributor.authorBujarrabal, Valentín-
dc.contributor.authorChu, Yoohua-
dc.contributor.authorCorradi, Romano L M-
dc.contributor.authorDe Marco, Orsola-
dc.contributor.authorFrank, A.-
dc.contributor.authorFreeman, M.-
dc.contributor.authorFrew, David J.-
dc.contributor.authorGuerrero, Martín Antonio-
dc.contributor.authorJones, David I.-
dc.contributor.authorĹopez, José Alberto-
dc.contributor.authorMiszalski, Brent-
dc.contributor.authorNordhaus, Jason T.-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorSahai, Raghvendra-
dc.contributor.authorSandin, Christer-
dc.contributor.authorSchönberner, Detlef-
dc.contributor.authorSoker, Noam-
dc.contributor.authorSokoloski, Jennifer L.-
dc.contributor.authorSteffen, Matthias-
dc.contributor.authorToalá, Jesús A.-
dc.contributor.authorUeta, Toshiya-
dc.contributor.authorVillaver, Eva V A-
dc.contributor.authorZijlstra, Albert A.-
dc.date.accessioned2015-03-23T02:31:17Z-
dc.date.available2015-03-23T02:31:17Z-
dc.date.issued2015-
dc.identifier.citationAstrophysical Journal Letters, 2015, v. 800, n. 1-
dc.identifier.issn2041-8205-
dc.identifier.urihttp://hdl.handle.net/10722/209045-
dc.description.abstract© 2015. The American Astronomical Society. All rights reserved. We present X-ray spectral analysis of 20 point-like X-ray sources detected in Chandra Planetary Nebula Survey observations of 59 planetary nebulae (PNe) in the solar neighborhood. Most of these 20 detections are associated with luminous central stars within relatively young, compact nebulae. The vast majority of these point-like X-ray-emitting sources at PN cores display relatively "hard" (≥0.5 keV) X-ray emission components that are unlikely to be due to photospheric emission from the hot central stars (CSPN). Instead, we demonstrate that these sources are well modeled by optically thin thermal plasmas. From the plasma properties, we identify two classes of CSPN X-ray emission: (1) high-temperature plasmas with X-ray luminosities, LX, that appear uncorrelated with the CSPN bolometric luminosity, L bol and (2) lower-temperature plasmas with L X/L bol 10-7. We suggest these two classes correspond to the physical processes of magnetically active binary companions and self-shocking stellar winds, respectively. In many cases this conclusion is supported by corroborative multiwavelength evidence for the wind and binary properties of the PN central stars. By thus honing in on the origins of X-ray emission from PN central stars, we enhance the ability of CSPN X-ray sources to constrain models of PN shaping that invoke wind interactions and binarity.-
dc.languageeng-
dc.relation.ispartofAstrophysical Journal Letters-
dc.subjectplanetary nebulae-
dc.subjectgeneral-
dc.titleThe chandra planetary nebula survey (chanplaNS). III. X-ray emission from the central stars of planetary nebulae-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1088/0004-637X/800/1/8-
dc.identifier.scopuseid_2-s2.0-84922578628-
dc.identifier.volume800-
dc.identifier.issue1-
dc.identifier.eissn2041-8213-

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