The ISO-Spectrum of the Young Star HD 100546

Malfait, K.; Waelkens, Christoffel; Vandenbussche, B.

doi:10.1007/978-94-011-5076-7_5

Cited by 28 publications

(37 citation statements)

References 16 publications

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“…Pantin (Waelkens) and Malfait et al (1999) have presented the observations from the CWAELKEN programs. We have reprocessed the three sets of observations with the latest pipeline software (compatible with the ISO pipeline OLP10.1) and interactive techniques to detect and correct the effects of cosmic radiation on the scan data and dark currents.…”

Section: Sws Observationsmentioning

confidence: 99%

The mid-infrared spectrum of the zodiacal and exozodiacal light

Reach

Morris

Boulanger

et al. 2003

Icarus

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The zodiacal light is the dominant source of the mid-infrared sky brightness seen from Earth, and exozodiacal light is the dominant emission from planetary and debris systems around other stars. We observed the zodiacal light spectrum with the midinfrared camera ISOCAM over the wavelength range 5-16 µm and a wide range of orientations relative to the Sun (solar elongations 68 • -113 • ) and the ecliptic (plane to pole). The temperature in the ecliptic ranged from 269 K at solar elongation 68 • to 244 K at 113 • , and the polar temperature, characteristic of dust 1 AU from the Sun, is 274 K. The observed temperature is exactly as expected for large (> 10µm radius), low-albedo (< 0.08), rapidly-rotating, grey particles 1 AU from the Sun. Smaller particles (< 10 µm radius) radiate inefficiently in the infrared and are warmer than observed. We present theoretical models for a wide range of particle size distributions and compositions; it is evident that the zodiacal light is produced by particles in the 10-100 µm radius range. In addition to the continuum, we detect a weak excess in the 9-11 µm range, with an amplitude of 6% of the continuum. The shape of the feature can be matched by a mixture of silicates: amorphous forsterite/olivine provides most of the continuum and some of the 9-11 µm silicate feature, dirty crystalline olivine provides the red wing of the silicate feature (and a bump at 11.35 µm), and a hydrous silicate (montmorillonite) provides the blue wing of the silicate feature. The presence of hydrous silicate suggests the parent bodies of those particles were formed in the inner solar nebula. Large particles dominate the size distribution, but at least some small particles (radii ∼ 1 µm) are required to produce the silicate emission feature. The strength of the feature may vary spatially, with the strongest features being at the lowest solar elongations as well as at high ecliptic latitudes; if confirmed, this would imply that the dust properties change such that dust further from the Sun has a weaker silicate feature.-2 -To compare the properties of zodiacal dust to dust around other main sequence stars, we reanalyzed the exozodiacal light spectrum for β Pic to derive the shape of its silicate feature. The zodiacal and exozodiacal spectra are very different. The exozodiacal spectra are dominated by cold dust, with emission peaking in the far-infrared, while the zodiacal spectrum peaks around 20 µm. We removed the debris disk continuum from the spectra by fitting a blackbody with a different temperature for each aperture (ranging from 3.7 ′′ to 27 ′′ ); the resulting silicate spectra for β Pic are identical for all apertures, indicating that the silicate feature arises close to the star. The shape of the silicate feature from β Pic is nearly identical to that derived from the ISO spectrum of 51 Oph; both exozodiacal features are very different from that of the zodiacal light. The exozodiacal features are roughly triangular, peaking at 10.3 µm, while the zodiacal feature is more boxy.

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Section: Sws Observationsmentioning

confidence: 99%

The mid-infrared spectrum of the zodiacal and exozodiacal light

Reach

Morris

Boulanger

et al. 2003

Icarus

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“…Malfait et al (1999) find no correlation between the spectral dust signatures (including crystallinity) and the stellar parameters such as age. More work is needed to clarify this important evolutionary issue and crystallize the theoretical thought.…”

Section: Hd 100546: Mineralogy Of Solids and Possible Cometary Activitymentioning

confidence: 72%

“…While we have no definite answers yet (global mixing or circulation in the nebula may be required), we note that this problem concerns in equal degree the partial crystallinity of comets in the solar system. In fact, as Malfait et al (1998; clearly show, in young planetary systems we are seeing dust very similar to the cometary dust. The lower graph in Fig.…”

Section: Hd 100546: Mineralogy Of Solids and Possible Cometary Activitymentioning

confidence: 78%

“…, and comet Hale-Bopp dust (lower curve). Emission features of crystalline forsterite, amorphous olivine, FeO, and PAH molecules have been identified in the disk spectrum (from Malfait et al, 1998).…”

Section: Hd 100546: Mineralogy Of Solids and Possible Cometary Activitymentioning

confidence: 99%

“…The system is ∼10 Myr old, and therefore belongs to the transitional IR-excess systems that may or may not have the primordial gas in the disk. Malfait et al (1998; obtained the SWS and LWS ISO spectra of the system. A variety of emission features of carbon-and oxygen-rich dust were found, most notably from crystalline forsterite.…”

Section: Hd 100546: Mineralogy Of Solids and Possible Cometary Activitymentioning

confidence: 99%

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Beta Pictoris and other Solar Systems

Artymowicz

2000

From Dust to Terrestrial Planets

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Abstract. Planetary systems come in a bewildering variety of shapes and sizes. In addition to the exoplanetary systems with giant planets, found in surveys of stellar radial velocity variations, an overlapping class of dusty disk-containing solar systems exists. The disks include large quantities of meteoroids and dust, and a varying complement of gas. Their solid material represents 'replenished' dust born in the collisions/sublimation of planetesimals perturbed by planets. We present several such systems, including HR 4796A, HD 141569, HD 100546, and the prototypical replenished disk of Beta Pictoris. We discuss the composition, physical processing, and migration of dust in the disks, their evolutionary status, and the evidence of embedded planets.

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