J/A+A/439/1149 XMM spectroscopy of TWA 5 (Argiroffi+, 2005)
XMM-Newton spectroscopy of the metal depleted T Tauri star TWA 5.
Argiroffi C., Maggio A., Peres G., Stelzer B., Neuhaeuser R.
<Astron. Astrophys., 439, 1149-1158 (2005)>
=2005A&A...439.1149A 2005A&A...439.1149A
ADC_Keywords: Stars, double and multiple ; Stars, pre-main sequence ;
X-ray sources ; Spectroscopy
Keywords: X-rays: stars - techniques: spectroscopic - stars: activity -
stars: abundances - stars: pre-main sequence -
stars: individual: TWA 5
Abstract:
We present results of X-ray spectroscopy for TWA 5, a member of the
young TW Hydrae association, observed with XMM-Newton. TWA 5 is a
multiple system which shows Hα emission, a signature typical
of classical T Tauri stars, but no infrared excess. From this analysis
of the RGS and EPIC spectra, we have derived the emission measure
distribution vs. temperature of the X-ray emitting plasma, its
abundances, and the electron density.
Description:
TWA 5 was observed for ∼30ks with XMM-Newton on January 9, 2003.
Objects:
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RA (2000) DE Designation(s)
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11 31 55.3 -34 36 27 TWA 5 = TYC 7223-275-1
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 106 53 Strongest RGS lines of TWA 5
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- Label Label number
5- 9 F5.2 0.1nm LambdaO ?=- Observed wavelength (1)
11- 17 F7.4 0.1nm LambdaP Predicted wavelength (1)
19- 27 A9 --- Ion Ion
29- 90 A62 --- Trans Transition (upper --> lower)
93- 96 F4.2 [K] logTmax Temperature of maximum emissivity
98-102 F5.1 10-6ph/s/cm2 Flux ? Line flux (2)
104-106 F3.1 10-6ph/s/cm2 e_Flux ? rms uncertainty on Flux (2)
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Note (1): Observed and predicted (APED database) wavelengths. In the cases
of unresolved blends identified by the same label number, we list
the main components in order of increasing predicted wavelength.
Note (2): Line fluxes with uncertainties at the 68% confidence level
obtained by fitting RGS1 and RGS2 spectra simultaneously. In the
cases of unresolved blends identified by the same label number,
we report only the total flux of the blended lines
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 27-Jul-2006