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J/A+A/365/545   Remnant disks around main-sequence stars IR flux (Habing+, 2001)

Incidence and survival of remnant disks around main-sequence stars Habing H.J., Dominik C., Jourdain de Muizon M., Laureijs R.J., Kessler M.F., Leech K., Metcalfe L., Siebenmorgen R., Trams N., Bouchet P. <Astron. Astrophys. 365, 545 (2001)> =2001A&A...365..545H
ADC_Keywords: Stars, dwarfs ; Infrared sources ; Photometry, UBV Keywords: stars: planetary systems - infrared: stars Abstract: We present photometric ISO 60 and 170µm measurements, complemented by some IRAS data at 60µm, of a sample of 84 nearby main-sequence stars of spectral class A, F, G and K in order to determine the incidence of dust disks around such main-sequence stars. Fifty stars were detected at 60µm; 36 of these emit a flux expected from their photosphere while 14 emit significantly more. The excess emission we attribute to a circumstellar disk like the ones around Vega and β Pictoris. Thirty four stars were not detected at all; the expected photospheric flux, however, is so close to the detection limit that the stars cannot have an excess stronger than the photospheric flux density at 60µm. Of the stars younger than 400Myr one in two has a disk; for the older stars this is true for only one in ten. We conclude that most stars arrive on the main sequence surrounded by a disk; this disk then decays in about 400Myr. Because (i) the dust particles disappear and must be replenished on a much shorter time scale and (ii) the collision of planetesimals is a good source of new dust, we suggest that the rapid decay of the disks is caused by the destruction and escape of planetesimals. We suggest that the dissipation of the disk is related to the heavy bombardment phase in our Solar System. Whether all stars arrive on the main sequence surrounded by a disk cannot be established: some very young stars do not have a disk. And not all stars destroy their disk in a similar way: some stars as old as the Sun still have significant disks. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 68 84 Basic data on all stars table3.dat 111 84 60 micron flux densities table4.dat 111 52 170 micron flux densities tables.tex 117 304 LaTeX version of the tables
See also: I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) III/135 : Henry Draper Catalogue and Extension (Cannon+ 1918-1924; ADC 1989) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD Star number in the Henry Draper Catalogue (Cat. III/135) 9- 14 I6 --- HIP ? Star number in the HIPPARCOS catalogue (Cat. I/239) 16- 30 A15 --- Name Stellar name 32- 36 F5.2 mag Vmag V-magnitude taken from the Geneva photometric catalogue 38- 42 F5.2 mag B-V B-V colour taken from the Geneva photometric catalogue 44- 47 F4.1 pc Dist Stellar distance, taken from the Hipparcos catalogue (I/239) 49- 57 A9 --- SpType Spectral type taken from the Hipparcos catalogue (I/239) 59- 63 F5.2 Gyr Age ? Stellar age 65- 68 I4 K Teff Effective temperature
Byte-by-byte Description of file: table3.dat table4.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD Star number in the Henry Draper Catalogue 9- 16 I8 --- ISO-ID ? Identification number of the measurement used in the ISO archive 18- 22 I5 mJy Fnu Flux density corrected for bandwidth effects (4) (1) 24- 26 I3 mJy e_Fnu Error on Fnu (4) (2) 28- 31 I4 mJy Fnup ? Flux expected from the stellar photosphere (see the text) (4) 33- 37 I5 mJy EFnu Excess flux (Fnu - Fnup) (4) (5) 39 A1 --- lEFnu/eFnu Limit flag on EFnu/e_Fnu 40- 43 F4.1 --- EFnu/e_Fnu Ratio of the excess flux compared to the measurement error 45- 49 I5 mJy Fnud ? Monochromatic excess flux density (3) 51 A1 --- l_log(tau)d Limit flag on log(tau)d 52- 55 F4.1 --- log(tau)d ? An estimate of the optical depth of the disk at visual wavelengths, but estimated from the flux density at 60 micron 57-111 A55 --- Ref Mode of observation reference (table3 only)
Note (1): Flux density corrected for bandwidth effects under the assumption that the spectrum is characterized by the Rayleigh-Jeans equation and for the fact that the stellar flux extended over more than 1 pixel. Note (2): Error estimate assigned by the ISOPHOT software to the flux measurement in the previous column; for IRAS measurements the error has been put at 100mJy. Note (3): Monochromatic excess flux density recalculated by assuming a flat spectrum within the ISOPHOT 60µm bandwidth; this is our estimate of the monochromatic flux density from the disk. Note (4): In table4.dat, fluxes are corrected for point spread function and Rayleigh-Jeans colour-correction, i.e. the inband flux has been divided by 0.64 (psf) and by 1.2 (cc). Note (5): In table4.dat, "de-colour-corrected" excess from Fnu.
Acknowledgements: Harm Habing
(End) Patricia Bauer CDS 24-Nov-2000
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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