CHANDRA REVEALS VARIABLE MULTI-COMPONENT X-RAY EMISSION FROM FU ORIONIS

Skinner, Stephen L; Guedel, Manuel; Briggs, Kevin R

doi:10.1088/0004-637X/722/2/1654

Title: CHANDRA REVEALS VARIABLE MULTI-COMPONENT X-RAY EMISSION FROM FU ORIONIS

Full Record
Other Related Research

Abstract

FU Orionis is the prototype of a class of eruptive young stars ('FUors') characterized by strong optical outbursts. We recently completed an exploratory survey of FUors using XMM-Newton to determine their X-ray properties, about which little was previously known. The prototype FU Ori and V1735 Cyg were detected. The X-ray spectrum of FU Ori was found to be unusual, consisting of a cool moderately absorbed component plus a hotter component viewed through an absorption column density that is an order of magnitude higher. We present here a sensitive (99 ks) follow-up X-ray observation of FU Ori obtained at higher angular resolution with Chandra ACIS-S. The unusual multi-component spectrum is confirmed. The hot component is centered on FU Ori and dominates the emission above 2 keV. It is variable (a signature of magnetic activity) and is probably coronal emission originating close to FU Ori's surface viewed through cool gas in FU Ori's strong wind or accretion stream. In contrast, the X-ray centroid of the soft emission below 2 keV is offset 0.''20 to the southeast of FU Ori, toward the near-IR companion (FU Ori S). This offset amounts to slightly less than half the separation between the two stars. The mostmore »« less

Authors:

Skinner, Stephen L ^[1]; Guedel, Manuel ^[2]; Briggs, Kevin R ^[3]

CASA, University of Colorado, Boulder, CO 80309-0389 (United States)
Department of Astronomy, University of Vienna, Tuerkenschanzstr. 17, A-1180 Vienna (Austria)
Institute of Astronomy, ETH Zuerich, Wolfgang-Pauli-Strasse 27, 8093 Zuerich (Switzerland)

Publication Date:: Wed Oct 20 00:00:00 EDT 2010

OSTI Identifier:: 21464588

Resource Type:: Journal Article

Journal Name:: Astrophysical Journal

Additional Journal Information:: Journal Volume: 722; Journal Issue: 2; Other Information: DOI: 10.1088/0004-637X/722/2/1654; Journal ID: ISSN 0004-637X

Country of Publication:: United States

Language:: English

Subject:: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; COSMIC X-RAY SOURCES; SOFT X RADIATION; STARS; X-RAY SPECTRA; COSMIC RAY SOURCES; ELECTROMAGNETIC RADIATION; IONIZING RADIATIONS; RADIATIONS; SORPTION; SPECTRA; X RADIATION

Citation Formats


                    Skinner, Stephen L, Guedel, Manuel, Briggs, Kevin R, and Lamzin, Sergei A., E-mail: stephen.skinner@colorado.ed. CHANDRA REVEALS VARIABLE MULTI-COMPONENT X-RAY EMISSION FROM FU ORIONIS.  United States: N. p., 2010. 
        Web.  doi:10.1088/0004-637X/722/2/1654.

Copy to clipboard


                    Skinner, Stephen L, Guedel, Manuel, Briggs, Kevin R, & Lamzin, Sergei A., E-mail: stephen.skinner@colorado.ed. CHANDRA REVEALS VARIABLE MULTI-COMPONENT X-RAY EMISSION FROM FU ORIONIS.  United States.  https://doi.org/10.1088/0004-637X/722/2/1654

Copy to clipboard


                    Skinner, Stephen L, Guedel, Manuel, Briggs, Kevin R, and Lamzin, Sergei A., E-mail: stephen.skinner@colorado.ed. 2010.  
        "CHANDRA REVEALS VARIABLE MULTI-COMPONENT X-RAY EMISSION FROM FU ORIONIS".  United States.  https://doi.org/10.1088/0004-637X/722/2/1654.

Copy to clipboard


                    
@article{osti_21464588,

  title        = {CHANDRA REVEALS VARIABLE MULTI-COMPONENT X-RAY EMISSION FROM FU ORIONIS},

  author       = {Skinner, Stephen L and Guedel, Manuel and Briggs, Kevin R and Lamzin, Sergei A., E-mail: stephen.skinner@colorado.ed},

  abstractNote = {FU Orionis is the prototype of a class of eruptive young stars ('FUors') characterized by strong optical outbursts. We recently completed an exploratory survey of FUors using XMM-Newton to determine their X-ray properties, about which little was previously known. The prototype FU Ori and V1735 Cyg were detected. The X-ray spectrum of FU Ori was found to be unusual, consisting of a cool moderately absorbed component plus a hotter component viewed through an absorption column density that is an order of magnitude higher. We present here a sensitive (99 ks) follow-up X-ray observation of FU Ori obtained at higher angular resolution with Chandra ACIS-S. The unusual multi-component spectrum is confirmed. The hot component is centered on FU Ori and dominates the emission above 2 keV. It is variable (a signature of magnetic activity) and is probably coronal emission originating close to FU Ori's surface viewed through cool gas in FU Ori's strong wind or accretion stream. In contrast, the X-ray centroid of the soft emission below 2 keV is offset 0.''20 to the southeast of FU Ori, toward the near-IR companion (FU Ori S). This offset amounts to slightly less than half the separation between the two stars. The most likely explanation for the offset is that the companion contributes significantly to the softer X-ray emission below 2 keV (and weakly above 2 keV). The superimposed X-ray contributions from FU Ori and the companion resolve the paradox posed by XMM-Newton of an apparently single X-ray source viewed through two different absorption columns.},

  doi          = {10.1088/0004-637X/722/2/1654},

  url          = {https://www.osti.gov/biblio/21464588},
  journal      = {Astrophysical Journal},

  issn         = {0004-637X},

  number       = 2,

  volume       = 722,

  place        = {United States},

  year         = {Wed Oct 20 00:00:00 EDT 2010},

  month        = {Wed Oct 20 00:00:00 EDT 2010}

}

Copy to clipboard

Journal Article:

https://doi.org/10.1088/0004-637X/722/2/1654

Other availability

Find in Google Scholar

Search WorldCat to find libraries that may hold this journal

Save / Share:

Export Metadata

Save to My Library

Similar records in OSTI.GOV collections:

AN ANALYSIS OF THE ENVIRONMENTS OF FU ORIONIS OBJECTS WITH HERSCHEL

Journal Article Green, Joel; Evans, II, Neal; Merello, Manuel; ... - Astrophysical Journal

We present Herschel-HIFI, SPIRE, and PACS 50-670 {mu}m imaging and spectroscopy of six FU Orionis-type objects and candidates (FU Orionis, V1735 Cyg, V1515 Cyg, V1057 Cyg, V1331 Cyg, and HBC 722), ranging in outburst date from 1936 to 2010, from the 'FOOSH' (FU Orionis Objects Surveyed with Herschel) program, as well as ancillary results from Spitzer Infrared Spectrograph and the Caltech Submillimeter Observatory. In their system properties (L{sub bol}, T{sub bol}, and line emission), we find that FUors are in a variety of evolutionary states. Additionally, some FUors have features of both Class I and II sources: warm continuum consistentmore »« less
https://doi.org/10.1088/0004-637X/772/2/117
X-RAY EMISSION FROM THE FU ORIONIS STAR V1735 CYGNI

Journal Article Skinner, Stephen; Sokal, Kimberly; Guedel, Manuel; ... - Astrophysical Journal

The variable star V1735 Cyg (=Elias 1-12) lies in the IC 5146 dark cloud and is a member of the class of FU Orionis objects whose dramatic optical brightenings are thought to be linked to episodic accretion. We report the first X-ray detections of V1735 Cyg and a deeply embedded class I protostar lying 24'' to its northeast. X-ray spectra obtained with EPIC on XMM-Newton reveal very high-temperature plasma (kT > 5 keV) in both objects, but no large flares. Such hard X-ray emission is not anticipated from accretion shocks and is a signature of magnetic processes. We place thesemore »« less
https://doi.org/10.1088/0004-637X/696/1/766; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)
RESOLVING THE SUB-AU-SCALE GAS AND DUST DISTRIBUTION IN FU ORIONIS SOURCES

Journal Article Eisner, J; Hillenbrand, L - Astrophysical Journal

We present Keck Interferometer observations of the three prototypical FU Orionis stars, FU Ori, V1057 Cyg, and V1515 Cyg. With a spatial resolution of a few milliarcseconds and a spectral resolution of {lambda}/{Delta}{lambda} = 2000, our near-infrared observations spatially resolve gas and dust emission extending from stellocentric radii of {approx}0.05 AU to several AU. We fit these data with accretion disk models where each stellocentric radius of the disk is represented by a supergiant-type stellar emission spectrum at the disk temperature. A disk model is consistent with the data for FU Ori, although we require some local asymmetry in themore »« less
https://doi.org/10.1088/0004-637X/738/1/9
Chandra Resolves the Double FU Orionis System RNO 1B/1C in X-Rays

Journal Article Skinner, Stephen; Güdel, Manuel - The Astronomical Journal (Online)

We present new Chandra X-ray observations of the close pair of young stars RNO 1B and 1C (6″ separation) located in the L1287 cloud. RNO 1B erupted in 1978–1990 and is classified as an FU Orionis star (FUor). RNO 1C also shows most of the properties of an FUor but no eruption has been seen yet. Only a few dozen FUors are known and the presence of two such objects with a small angular separation is rare, suggesting a common origin. Both stars were faintly detected by Chandra and we summarize their X-ray properties within the framework of other previouslymore »« less
https://doi.org/10.3847/1538-3881/AB846B
Ring-shaped nebulae around FU Orionis stars

Journal Article Goodrich, R - Publ. Astron. Soc. Pac.; (United States)

Observational data on the morphology and spectra of the nebulae surrounding V1057 Cyg, V1515 Cyg, and V1735 Cyg stars are presented and studied. The data reveal that V1735 Cyg is more highly reddened than the nebula and the spectra of all three nebulae are from reflection. A simple model for the dust shell is proposed and it is argued that the shells may indicate a relatively advanced evolutionary state for the FU Orionis star. The relation between the shells and the evolution of the stars is examined. The models of Herbig (1977), Mould et al. (1978), Larson (1980), and Hartmannmore »« less
https://doi.org/10.1086/131963

Similar Records