The absence of CO from the dust peak around e Eri

IM Coulson; WRF Dent; Jane Sophia Greaves

doi:10.1111/j.1365-2966.2004.07563.x

The absence of CO from the dust peak around e Eri

IM Coulson, WRF Dent, Jane Sophia Greaves

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

We have searched for the J = 2-1 emission of carbon monoxide (CO) from the brightest peak in the epsilon Eridani (epsilon Eri) dust disc - without success. The non-detection sets 3sigma upper limits to the mass of CO gas in the dust peak of 3.3 x 10(16) kg and to the total amount of (H-2) gas in the disc of 8 x 10(19) kg. The paucity of gas in the disc (there is similar to1000x more dust) constrains the composition of orbiting comets or icy planetesimals. If these comprise the pre-eminent reservoir of dust and gas in both the Edgeworth-Kuiper Belt (EKB) and the epsilon Eri disc then it seems unlikely that the epsilon Eri planetesimals can be as rich in volatiles as their EKB counterparts.

Original language	English
Pages (from-to)	L39-L42
Number of pages	4
Journal	Monthly Notices of the Royal Astronomical Society
Volume	348
Issue number	3
DOIs	https://doi.org/10.1111/j.1365-2966.2004.07563.x
Publication status	Published - 1 Mar 2004

Keywords

Kuiper Belt
circumstellar matter
stairs : individual : epsilon Eri
EDGEWORTH-KUIPER BELT
VEGA-EXCESS STARS
GIANT PLANETS
MOLECULAR-HYDROGEN
THERMAL EVOLUTION
BETA-PICTORIS
DEBRIS DISKS
SUBMILLIMETER
ERIDANI
GAS

Access to Document

10.1111/j.1365-2966.2004.07563.x

Cite this

@article{c33fef3753ea4617989806108e8d3790,

title = "The absence of CO from the dust peak around e Eri",

abstract = "We have searched for the J = 2-1 emission of carbon monoxide (CO) from the brightest peak in the epsilon Eridani (epsilon Eri) dust disc - without success. The non-detection sets 3sigma upper limits to the mass of CO gas in the dust peak of 3.3 x 10(16) kg and to the total amount of (H-2) gas in the disc of 8 x 10(19) kg. The paucity of gas in the disc (there is similar to1000x more dust) constrains the composition of orbiting comets or icy planetesimals. If these comprise the pre-eminent reservoir of dust and gas in both the Edgeworth-Kuiper Belt (EKB) and the epsilon Eri disc then it seems unlikely that the epsilon Eri planetesimals can be as rich in volatiles as their EKB counterparts.",

keywords = "Kuiper Belt, circumstellar matter, stairs : individual : epsilon Eri, EDGEWORTH-KUIPER BELT, VEGA-EXCESS STARS, GIANT PLANETS, MOLECULAR-HYDROGEN, THERMAL EVOLUTION, BETA-PICTORIS, DEBRIS DISKS, SUBMILLIMETER, ERIDANI, GAS",

author = "IM Coulson and WRF Dent and Greaves, \{Jane Sophia\}",

year = "2004",

month = mar,

day = "1",

doi = "10.1111/j.1365-2966.2004.07563.x",

language = "English",

volume = "348",

pages = "L39--L42",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

TY - JOUR

T1 - The absence of CO from the dust peak around e Eri

AU - Coulson, IM

AU - Dent, WRF

AU - Greaves, Jane Sophia

PY - 2004/3/1

Y1 - 2004/3/1

N2 - We have searched for the J = 2-1 emission of carbon monoxide (CO) from the brightest peak in the epsilon Eridani (epsilon Eri) dust disc - without success. The non-detection sets 3sigma upper limits to the mass of CO gas in the dust peak of 3.3 x 10(16) kg and to the total amount of (H-2) gas in the disc of 8 x 10(19) kg. The paucity of gas in the disc (there is similar to1000x more dust) constrains the composition of orbiting comets or icy planetesimals. If these comprise the pre-eminent reservoir of dust and gas in both the Edgeworth-Kuiper Belt (EKB) and the epsilon Eri disc then it seems unlikely that the epsilon Eri planetesimals can be as rich in volatiles as their EKB counterparts.

AB - We have searched for the J = 2-1 emission of carbon monoxide (CO) from the brightest peak in the epsilon Eridani (epsilon Eri) dust disc - without success. The non-detection sets 3sigma upper limits to the mass of CO gas in the dust peak of 3.3 x 10(16) kg and to the total amount of (H-2) gas in the disc of 8 x 10(19) kg. The paucity of gas in the disc (there is similar to1000x more dust) constrains the composition of orbiting comets or icy planetesimals. If these comprise the pre-eminent reservoir of dust and gas in both the Edgeworth-Kuiper Belt (EKB) and the epsilon Eri disc then it seems unlikely that the epsilon Eri planetesimals can be as rich in volatiles as their EKB counterparts.

KW - Kuiper Belt

KW - circumstellar matter

KW - stairs : individual : epsilon Eri

KW - EDGEWORTH-KUIPER BELT

KW - VEGA-EXCESS STARS

KW - GIANT PLANETS

KW - MOLECULAR-HYDROGEN

KW - THERMAL EVOLUTION

KW - BETA-PICTORIS

KW - DEBRIS DISKS

KW - SUBMILLIMETER

KW - ERIDANI

KW - GAS

UR - http://www.blackwell-synergy.com/journals/resolver.asp?bibcode=2004MNRAS.348L..39C&format=

UR - https://www.scopus.com/pages/publications/1542327754

U2 - 10.1111/j.1365-2966.2004.07563.x

DO - 10.1111/j.1365-2966.2004.07563.x

M3 - Article

SN - 0035-8711

VL - 348

SP - L39-L42

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

The absence of CO from the dust peak around e Eri

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this