A Possible Massive Asteroid Belt around ζ Leporis

Chen, Christine; Jura, M.

doi:10.1086/324057

Cited by 72 publications

(74 citation statements)

References 15 publications

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“…where N(a) is the number of particles per cm 3 with radii between a and a þ da (see, e.g., Dohnanyi 1969;Williams & Wetherill 1994;Chen & Jura 2001). The smallest particle radius in this distribution may be set by radiation pressure blowout; for the mass (1.35 M ) and luminosity (2.8 L ) we estimate for HD 23514, this radius is $0.5 m.…”

Section: Discussionmentioning

confidence: 89%

“…In addition to collisions, PR drag and stellar wind drag are loss mechanisms for small dust particles. The timescale for PR drag at HD 23514 may be evaluated using, for example, equation (5) in Chen & Jura (2001). We assume L Ã ¼ 2:8 L (corresponding to a distance of 130 pc to HD 23514), a dust particle orbital semimajor axis of 1 AU, and a radius and density of a typical individual grain to be 1 m and 2.5 g cm À3 , respectively.…”

Section: Discussionmentioning

confidence: 99%

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Warm Dust in the Terrestrial Planet Zone of a Sun‐like Pleiades Star: Collisions between Planetary Embryos?

Rhee

Song

Zuckerman

2008

ApJ

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Only a few solar-type main-sequence stars are known to be orbited by warm dust particles; the most extreme is the G0 field star BD +20 307 that emits $4% of its energy at mid-infrared wavelengths. We report the identification of a similarly dusty star HD 23514, an F6-type member of the Pleiades. A strong mid-IR silicate emission feature indicates the presence of small warm dust particles, but with the primary flux density peak at the nonstandard wavelength of $9 m. The existence of so much dust within an AU or so of these stars is not easily accounted for given the very brief lifetime in orbit of small particles. The apparent absence of very hot ( k1000 K ) dust at both stars suggests the possible presence of a planet closer to the stars than the dust. The observed frequency of the BD +20 307/ HD 23514 phenomenon indicates that the mass equivalent of Earth's Moon must be converted, via collisions of massive bodies, to tiny dust particles that find their way to the terrestrial planet zone during the first few hundred million years of the life of many (most?) Sun-like stars. Identification of these two dusty systems among youthful nearby solar-type stars suggests that terrestrial planet formation is common.

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Section: Discussionmentioning

confidence: 89%

Section: Discussionmentioning

confidence: 99%

Warm Dust in the Terrestrial Planet Zone of a Sun‐like Pleiades Star: Collisions between Planetary Embryos?

Rhee

Song

Zuckerman

2008

ApJ

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“…where Q P R is the radiation pressure coupling coefficient and ρ is the density of a typical dust particle (Chen & Jura 2001). We assume Q P R ∼1 for 2πa/λ > 1 and ρ∼2.5 g cm −3 .…”

Section: Dust Parametersmentioning

confidence: 99%

Herschel Observations of Dusty Debris Disks

Vican

Schneider

Bryden

et al. 2016

ApJ

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We present results from two Herschel observing programs using the Photodetector Array Camera and Spectrometer. During three separate campaigns, we obtained Herschel data for 24 stars at 70, 100, and 160 µm. We chose stars that were already known or suspected to have circumstellar dust based on excess infrared emission previously measured with IRAS or Spitzer, and used Herschel to examine long-wavelength properties of the dust. Fifteen stars were found to be uncontaminated by background sources, and possess infrared emission most likely due to a circumstellar debris disk. We analyzed the properties of these debris disks to better understand the physical mechanisms responsible for dust production and removal. Seven targets were spatially resolved in the Herschel images. Based on fits to their spectral energy distributions, nine disks appear to have two temperature components. Of these nine, in three cases, the warmer dust component is likely the result of a transient process rather than a steady state collisional cascade. The dust belts at four stars are likely stirred by an unseen planet, and merit further investigation.

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“…We hypothesize that each system possesses at least as much mass in parent bodies today as that which would have been destroyed if the system were in steady state during the lifetime of the star. If M PB denotes the mass in parent bodies, then we may write (Chen & Jura 2001). If the disk is dominated by collisions, as is probably the case, then this estimate will be a lower bound.…”

Section: Dust Grain Propertiesmentioning

confidence: 99%

ASPITZERMIPS STUDY OF 2.5-2.0M_☉STARS IN SCORPIUS-CENTAURUS

Chen

Pecaut

Mamajek

et al. 2012

ApJ

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We have obtained Spitzer Space Telescope Multiband Imaging Photometer for Spitzer (MIPS) 24 μm and 70 μm observations of 215 nearby, Hipparcos B-and A-type common proper-motion single and binary systems in the nearest OB association, Scorpius-Centaurus. Combining our MIPS observations with those of other ScoCen stars in the literature, we estimate 24 μm B+A-type disk fractions of 17/67 (25 +6 −5 %), 36/131 (27 +4 −4 %), and 23/95 (24 +5 −4 %) for Upper Scorpius (∼11 Myr), Upper Centaurus Lupus (∼15 Myr), and Lower Centaurus Crux (∼17 Myr), respectively, somewhat smaller disk fractions than previously obtained for F-and G-type members. We confirm previous IRAS excess detections and present new discoveries of 51 protoplanetary and debris disk systems, with fractional infrared luminosities ranging from L IR /L * = 10 −6 to 10 −2 and grain temperatures ranging from T gr = 40 to 300 K. In addition, we confirm that the 24 μm and 70 μm excesses (or fractional infrared luminosities) around B+A-type stars are smaller than those measured toward F+G-type stars and hypothesize that the observed disk property dependence on stellar mass may be the result of a higher stellar companion fraction around B-and A-type stars at 10-200 AU. Finally, we note that the majority of the ScoCen 24 μm excess sources also possess 12 μm excess, indicating that Earth-like planets may be forming via collisions in the terrestrial planet zone at ∼10-100 Myr.

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A Possible Massive Asteroid Belt around ζ Leporis

Cited by 72 publications

References 15 publications

Warm Dust in the Terrestrial Planet Zone of a Sun‐like Pleiades Star: Collisions between Planetary Embryos?

Warm Dust in the Terrestrial Planet Zone of a Sun‐like Pleiades Star: Collisions between Planetary Embryos?

Herschel Observations of Dusty Debris Disks

ASPITZERMIPS STUDY OF 2.5-2.0M_☉STARS IN SCORPIUS-CENTAURUS

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A Possible Massive Asteroid Belt around ζ Leporis

Cited by 72 publications

References 15 publications

Warm Dust in the Terrestrial Planet Zone of a Sun‐like Pleiades Star: Collisions between Planetary Embryos?

Warm Dust in the Terrestrial Planet Zone of a Sun‐like Pleiades Star: Collisions between Planetary Embryos?

Herschel Observations of Dusty Debris Disks

ASPITZERMIPS STUDY OF 2.5-2.0M☉STARS IN SCORPIUS-CENTAURUS

Contact Info

Product

Resources

About

ASPITZERMIPS STUDY OF 2.5-2.0M_☉STARS IN SCORPIUS-CENTAURUS