High-Resolution X-Ray Spectroscopy of the Post-T Tauri Star PZ Telescopii

Giovanni Peres, Costanza Argiroffi, Antonio Maggio, Harnden, Sciortino, Drake

Risultato della ricerca: Article

24 Citazioni (Scopus)

Abstract

We present an analysis of the Chandra High Energy Transmission Grating Spectrometer observation of the rapidly rotating (Prot=0.94days) post-T Tauri (~20 Myr old) star PZ Telescopii, in the Tucana association. Using two different methods, we have derived the coronal emission measure distribution EM(T) and chemical abundances. The EM(T) peaks at logT=6.9 and exhibits a significant emission measure at temperatures logT>7. The coronal abundances are generally ~0.5 times the solar photospheric values, which are presumed fairly representative of the composition of the underlying star. A minimum in abundance is seen at a first ionization potential (FIP) of 7-8 eV, with evidence for higher abundances at both lower and higher FIP, similar to patterns seen in other active stars. From an analysis of the He-like triplet of Mg XI, we have estimated electron densities of ~10^12-10^13 cm^-3. All the coronal properties found for PZ Tel are much more similar to those of AB Dor, which is slightly older than PZ Tel, than to those of the younger T Tauri star TW Hya. These results support earlier conclusions that the soft X-ray emission of TW Hya is likely dominated by accretion activity rather than by a magnetically heated corona. Our results also suggest that the coronae of pre-main-sequence stars rapidly become similar to those of older active main-sequence stars soon after the accretion stage has ended.
Lingua originaleEnglish
pagine (da-a)925-934
Numero di pagine10
RivistaTHE ASTROPHYSICAL JOURNAL
Volume609
Stato di pubblicazionePublished - 2004

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T Tauri stars
X-ray spectroscopy
high resolution
stars
ionization potentials
spectroscopy
coronas
corona
ionization
x rays
accretion
pre-main sequence stars
main sequence stars
electron density
spectrometer
gratings
spectrometers
energy
temperature
analysis

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cita questo

High-Resolution X-Ray Spectroscopy of the Post-T Tauri Star PZ Telescopii. / Peres, Giovanni; Argiroffi, Costanza; Maggio, Antonio; Harnden; Sciortino; Drake.

In: THE ASTROPHYSICAL JOURNAL, Vol. 609, 2004, pag. 925-934.

Risultato della ricerca: Article

Peres, Giovanni ; Argiroffi, Costanza ; Maggio, Antonio ; Harnden ; Sciortino ; Drake. / High-Resolution X-Ray Spectroscopy of the Post-T Tauri Star PZ Telescopii. In: THE ASTROPHYSICAL JOURNAL. 2004 ; Vol. 609. pagg. 925-934.
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title = "High-Resolution X-Ray Spectroscopy of the Post-T Tauri Star PZ Telescopii",
abstract = "We present an analysis of the Chandra High Energy Transmission Grating Spectrometer observation of the rapidly rotating (Prot=0.94days) post-T Tauri (~20 Myr old) star PZ Telescopii, in the Tucana association. Using two different methods, we have derived the coronal emission measure distribution EM(T) and chemical abundances. The EM(T) peaks at logT=6.9 and exhibits a significant emission measure at temperatures logT>7. The coronal abundances are generally ~0.5 times the solar photospheric values, which are presumed fairly representative of the composition of the underlying star. A minimum in abundance is seen at a first ionization potential (FIP) of 7-8 eV, with evidence for higher abundances at both lower and higher FIP, similar to patterns seen in other active stars. From an analysis of the He-like triplet of Mg XI, we have estimated electron densities of ~10^12-10^13 cm^-3. All the coronal properties found for PZ Tel are much more similar to those of AB Dor, which is slightly older than PZ Tel, than to those of the younger T Tauri star TW Hya. These results support earlier conclusions that the soft X-ray emission of TW Hya is likely dominated by accretion activity rather than by a magnetically heated corona. Our results also suggest that the coronae of pre-main-sequence stars rapidly become similar to those of older active main-sequence stars soon after the accretion stage has ended.",
author = "Giovanni Peres and Costanza Argiroffi and Antonio Maggio and Harnden and Sciortino and Drake",
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TY - JOUR

T1 - High-Resolution X-Ray Spectroscopy of the Post-T Tauri Star PZ Telescopii

AU - Peres, Giovanni

AU - Argiroffi, Costanza

AU - Maggio, Antonio

AU - Harnden, null

AU - Sciortino, null

AU - Drake, null

PY - 2004

Y1 - 2004

N2 - We present an analysis of the Chandra High Energy Transmission Grating Spectrometer observation of the rapidly rotating (Prot=0.94days) post-T Tauri (~20 Myr old) star PZ Telescopii, in the Tucana association. Using two different methods, we have derived the coronal emission measure distribution EM(T) and chemical abundances. The EM(T) peaks at logT=6.9 and exhibits a significant emission measure at temperatures logT>7. The coronal abundances are generally ~0.5 times the solar photospheric values, which are presumed fairly representative of the composition of the underlying star. A minimum in abundance is seen at a first ionization potential (FIP) of 7-8 eV, with evidence for higher abundances at both lower and higher FIP, similar to patterns seen in other active stars. From an analysis of the He-like triplet of Mg XI, we have estimated electron densities of ~10^12-10^13 cm^-3. All the coronal properties found for PZ Tel are much more similar to those of AB Dor, which is slightly older than PZ Tel, than to those of the younger T Tauri star TW Hya. These results support earlier conclusions that the soft X-ray emission of TW Hya is likely dominated by accretion activity rather than by a magnetically heated corona. Our results also suggest that the coronae of pre-main-sequence stars rapidly become similar to those of older active main-sequence stars soon after the accretion stage has ended.

AB - We present an analysis of the Chandra High Energy Transmission Grating Spectrometer observation of the rapidly rotating (Prot=0.94days) post-T Tauri (~20 Myr old) star PZ Telescopii, in the Tucana association. Using two different methods, we have derived the coronal emission measure distribution EM(T) and chemical abundances. The EM(T) peaks at logT=6.9 and exhibits a significant emission measure at temperatures logT>7. The coronal abundances are generally ~0.5 times the solar photospheric values, which are presumed fairly representative of the composition of the underlying star. A minimum in abundance is seen at a first ionization potential (FIP) of 7-8 eV, with evidence for higher abundances at both lower and higher FIP, similar to patterns seen in other active stars. From an analysis of the He-like triplet of Mg XI, we have estimated electron densities of ~10^12-10^13 cm^-3. All the coronal properties found for PZ Tel are much more similar to those of AB Dor, which is slightly older than PZ Tel, than to those of the younger T Tauri star TW Hya. These results support earlier conclusions that the soft X-ray emission of TW Hya is likely dominated by accretion activity rather than by a magnetically heated corona. Our results also suggest that the coronae of pre-main-sequence stars rapidly become similar to those of older active main-sequence stars soon after the accretion stage has ended.

UR - http://hdl.handle.net/10447/33127

M3 - Article

VL - 609

SP - 925

EP - 934

JO - THE ASTROPHYSICAL JOURNAL

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