dc.creator |
Winn, Joshua N. |
|
dc.creator |
Matthews, Jaymie M. |
|
dc.creator |
Dawson, Rebekah I. |
|
dc.creator |
Fabrycky, Daniel |
|
dc.creator |
Holman, Matthew J. |
|
dc.creator |
Kallinger, Thomas |
|
dc.creator |
Kuschnig, Rainer |
|
dc.creator |
Sasselov, Dimitar |
|
dc.creator |
Dragomir, Diana |
|
dc.creator |
Guenther, David B. |
|
dc.date.accessioned |
2018-06-04T16:25:40Z |
|
dc.date.available |
2018-06-04T16:25:40Z |
|
dc.date.issued |
2011-08-10 |
|
dc.identifier.issn |
2041-8205 |
|
dc.identifier.uri |
http://library2.smu.ca/handle/01/27538 |
|
dc.description |
Publisher's Version/PDF |
|
dc.description.abstract |
We have detected transits of the innermost planet “e” orbiting 55 Cnc (V = 6.0), based on two weeks of nearly continuous photometric monitoring with the MOST space telescope. The transits occur with the period (0.74 days) and phase that had been predicted by Dawson & Fabrycky, and with the expected duration and depth for the crossing of a Sun-like star by a hot super-Earth. Assuming the star’s mass and radius to be 0.963<sup>+0.051</sup> <sub>−0.029 </sub>M<sub>☉</sub> and 0.943±0.010 R<sub>☉</sub>, the planet’s mass, radius, and mean density are 8.63±0.35 M<sub>⊕</sub>, 2.00±0.14 R<sub>⊕</sub>, and 5.9<sup>+1.5</sup> <sub>−1.1</sub> g cm<sup>−3</sup>, respectively. The mean density is comparable to that of Earth, despite the greater mass and consequently greater compression of the interior of 55 Cnc e. This suggests a rock-iron composition supplemented by a significant mass of water, gas, or other light elements. Outside of transits, we detected a sinusoidal signal resembling the expected signal due to the changing illuminated phase of the planet, but with a full range (168 ± 70 ppm) too large to be reflected light or thermal emission. This signal has no straightforward interpretation and should be checked with further observations. The host star of 55 Cnc e is brighter than that of any other known transiting planet, which will facilitate future investigations. |
en_CA |
dc.description.provenance |
Submitted by Betty McEachern (betty.mceachern@smu.ca) on 2018-06-04T16:25:40Z
No. of bitstreams: 1
Guenther_David_B_article_2011_b.pdf: 3323658 bytes, checksum: ac94e2c637327327e6344d41e9660b8c (MD5) |
en |
dc.description.provenance |
Made available in DSpace on 2018-06-04T16:25:40Z (GMT). No. of bitstreams: 1
Guenther_David_B_article_2011_b.pdf: 3323658 bytes, checksum: ac94e2c637327327e6344d41e9660b8c (MD5)
Previous issue date: 2011-08-10 |
en |
dc.language.iso |
en |
en_CA |
dc.publisher |
IOP Publishing Limited |
en_CA |
dc.relation.uri |
https://dx.doi.org/10.1088/2041-8205/737/1/L18 |
|
dc.rights |
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user. |
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dc.subject.lcsh |
Planetary systems |
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dc.subject.lcsh |
Satellites |
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dc.subject.lcsh |
Transits |
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dc.title |
A super-Earth transiting a naked-eye star |
en_CA |
dc.type |
Text |
en_CA |
dcterms.bibliographicCitation |
Astrophysical Journal Letters 737(1), L18. (2011) |
en_CA |
Copyright statement:
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.