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| {{Starbox begin
| | There's no incertitude that Google is comely a full-mature hardware company, merely the up-to-the-minute Google X cast is a stack dissimilar that tablets and smartphones ??�the companion hardly announced that it's edifice a "smart contact lens." However, it's non meant to be a miniaturized variant of Chalk ?? it's meant to aid diabetes patients sustenance cross of their glucose levels. Interior the genus Lens is a miniaturized radio receiver chip off and glucose monitor that leave mensurate the glucose levels of the wearer's tears. |
| | name = HD 114613
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| }}
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| {{Starbox image
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| | image =
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| <div style="position: relative">[[File:Centaurus IAU.svg|250px|alt=Diagram showing star positions and boundaries of the constellation of Centaurus and its surroundings]]
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| <div style="position: absolute; left: 113px; top: 74px">[[File:Cercle rouge 100%.svg|9px]]</div>
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| </div>
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| | caption = A [[star chart]] of the constellation of Centaurus showing the position of HD 114613.
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| }}
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| {{Starbox observe
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| | epoch = J2000.0
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| | constell = [[Centaurus]]
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| | ra = {{RA|13|12|03.19}}<ref name="van Leeuwen2007"/>
| |
| | dec = {{DEC|-37|48|10.89}}<ref name="van Leeuwen2007"/>
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| | appmag_v = 4.852 ± 0.011<ref name="Hog2000"/>
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| }}
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| {{Starbox character
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| | class = G3IV<ref name="Teff"/><ref group="note">Though SIMBAD references the star as G3V, The star is significantly over-luminous for a dwarf: on the Hertzsprung-Russell diagram (see image) the star lies on the subgiant band, so it listed as a subgiant here.</ref>
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| | b-v = 0.659 ± 0.020<ref name="Hog2000"/>
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| }}
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| {{Starbox astrometry
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| | radial_v = -15.0 ± 0.9
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| | prop_mo_ra = -381.72 ± 0.31<ref name="van Leeuwen2007"/>
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| | prop_mo_dec = 45.75 ± 0.20<ref name="van Leeuwen2007"/>
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| | parallax = 48.38
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| | p_error = 0.29
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| | parallax_footnote = <ref name="van Leeuwen2007"/>
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| | absmag_v = 3.276 ± 0.024<ref name="AbsMag"/>
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| }}
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| {{Starbox detail
| |
| | mass = 1.25 ± 0.03<ref name="Takeda2007"/>
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| | radius = 2.01 ± 0.06<ref name="Takeda2007"/>
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| | luminosity = 4.057 ± 0.014<ref name="Sousa08"/>
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| | gravity = 3.97 ± 0.02<ref name="Sousa08"/>
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| | temperature = 5729 ± 17<ref name="Sousa08"/>
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| | metal_fe = 0.19 ± 0.01<ref name="Sousa08"/>
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| | rotation = 34.1 ± 3.5 days<ref name="Lovis2011"/>
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| | rotational_velocity = 2.4 ± 0.5<ref name="Valenti2005"/>
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| | age_gyr = 5.20 ± 0.24<ref name="Takeda2007"/>
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| }}
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| {{Starbox catalog
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| | names = HIP 64408, Gliese 501.2, HR 4979
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| }}
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| {{Starbox reference
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| | Simbad = HD+114613
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| }}
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| {{Starbox end}}
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|
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|
| '''HD 114613''' ('''Gliese 501.2''') is a fifth magnitude yellow [[subgiant]] that lies approximately 67 [[light-year]]s away in the [[constellation]] of [[Centaurus]]. The star is host to a long-period giant planet, and may possibly be orbited by more. | | Google's hoping that it'll be a less terrible and encroaching way of life to monitor lizard glucose levels than the distinctive method acting of pricking a digit and examination pedigree droplets multiple multiplication a sidereal day. Ideally, the detector would be able-bodied to sire a version one time per second, and Google wants it to roleplay as an early word of advice device for when glucose levels kickoff dropping ?? the troupe imagines putt a small [http://www.ledilluminate.net LED illuminate] in the crystalline lens that could argue levels dropping supra or down the stairs a prepare doorstep. |
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| == Stellar characteristics ==
| | It's not a New idea for co-Divine Babek Parviz ?? backrest in 2009,�Parviz showed Wired a connected inter-group communication electron lens meant to measuring vital signs. And piece this is fresh run aground for Google, the estimate of a attached meet genus Lens for specifically measure glucose levels isn't Modern ?? Microsoft and the University of Washington�worked on a standardized contrive rearward in 2011. Both Parviz and gent co-fall flat Brian Elisha Graves Otis were at the University of Washington and contributed to that project, as intimately. |
| <div style="position: relative">[[File:HRDiagram.png|thumb|left|The position of HD 114613 on the [[Hertzsprung-Russell diagram]]. The star lies significantly above the main sequence.]]
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| <div style="position: absolute; left: 86px; top: 114px">[[File:Chess tile xg.svg|20px]]</div>
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| </div>
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| HD 114613 is a bright star that lies about eight arcminutes south-east of [[Iota Centauri]], towards the middle of Centaurus. Though it is fairly easily observable with the naked eye, the star does not have a [[Bayer designation|Bayer]] or [[Flamsteed designation|Flamsteed]] designation as the constellation of Centaurus contains many brighter stars.
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| The B-V colour and spectroscopic temperature of HD 114613 indicate that it has a spectral type of G3. This means that the star is only 50 [[kelvin]] cooler than the Sun, giving it the yellow hue typical of G-type stars. On the [[Hertzsprung-Russell diagram]] (left) the star lies significantly above the main sequence, and is close to the [[subgiant]] branch; this means that HD 114613 has depleted the hydrogen in its core through [[nuclear fusion]], and is increasing in luminosity and radius while decreasing in temperature as it moves towards the giant branch. The cooling of the star as it evolves means that it had an earlier spectral type when on the main sequence, probably close to the F9V [[Iota Horologii]].
| | Of course, this send off is hush a estimable ways polish off from existence a realness ?? Google says its operative with the Food and Drug Administration and is also looking for for early partners World Health Organization are "experts in bringing products like this to market." The company wants partners to apply its technology to grow these lenses and as well establish apps to shuffling the measurements useable to users. There's no Word of God on when this lense mightiness be a reality, or even if it'll sour as planned, only it's sound to [http://www.alexa.com/search?q=project&r=topsites_index&p=bigtop project] Google victimization its technology art to examine and work a long-standing aesculapian trouble.<br><br>If you have any questions concerning in which and how to use [http://batuiti.com/shop/iphone-5-5s-5c/spigen-sgp-slim-armor-case-for-iphone-5-5s-5g-cover/ slim armor], you can call us at the web-site. |
| | |
| As HD 114613 is ending hydrogen fusion, the star must be fairly old. When combined with a spectroscopically-derived mass of 1.25 ± 0.03 M<sub>☉</sub> and a surface gravity of log 3.95 ± 0.03 g the implied age of the star is 5.20 ± 0.24 billion years,<ref name="Takeda2007"/> making it slightly older than the Sun. Though stellar metallicities typically decrease with increasing stellar age, within the age range of the [[thin disk]] a wide range of metallicities are common; HD 114613's high iron abundance of 0.19 ± 0.01 dex (155 ± 4% of the solar abundance) is therefore not unusual. The rate of giant planet occurrence for Fe/H = 0.2 dex stars is about 15%,<ref name="Mortier2013"/> which makes it fairly unsurprising that the star hosts a giant planet.
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| Somewhat peculiarly for a star that both had an earlier spectral type than the Sun and is currently a subgiant, HD 114613 has a magnetic cycle.<ref name="Lovis2011"/> With a period of 897 ± 61 days, the star's magnetic cycle is about four-and-a-half times shorter than the [[Solar cycle|Solar magnetic cycle]] and is one of the shortest magnetic cycles known.
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| == Planet searches ==
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| Being bright and solar-type, HD 114613 is an attractive target for radial velocity (RV)-based planet searches.
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| HD 114613 was one of the 37 targets of the first RV-based planet search in the southern hemisphere, the [[ESO]]-CES survey that spanned between 1992 and 1998.<ref name="Endl2002"/> This survey did not detect any companion with several Jovian masses out to a few AU. An extension of this survey to the [[High Accuracy Radial Velocity Planet Searcher|HARPS]] spectrograph provides further constraint, suggesting that there are no Jupiter-mass companions out to about 5 AU.<ref name="Zechmeister2013"/>
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| HD 114613 is included in the samples of the ESO-[[CORALIE spectrograph|CORALIE]]<ref name="Mortier2013"/> and [[Anglo-Australian Telescope|AAT]]-UCLES<ref name="Jones2002"/> planet searches that both began in 1998. Seemingly finding the star to be RV-stable and suitable for higher precision, HD 114613 was included in a subset of the CORALIE sample that became the sample of the ESO-HARPS high precision planet search that began in 2004,<ref name="Sousa08"/> while the star was elevated in importance in the AAT sample in 2005.<ref name="Wittenmyer2010"/><ref name="Wittenmyer2011"/> Though apparently not included in its main sample, HD 114613 is included in the sample of the [[W. M. Keck Observatory|Keck]]-HIRES Eta-Earth low-mass planet search that also began in 2004.<ref name="Howard2010"/>
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| === Planetary system ===
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| In Wittenmyer et al. 2012,<ref name="Wittenmyer2012"/> HD 114613 is indicated to be a low-mass planet host. Though this references a Tuomi et al. 2012 (''Tuomi, M., et al. 2012, MNRAS, submitted''), no such paper was published that year. More recently, in a Tuomi et al. 2013,<ref name=Tuomi2013/> [[Tau Ceti]] is noted to have a similar activity index distribution to HD 114613. Again, a Tuomi et al. 2012 is referenced, though somewhat more completely (''Tuomi, M., Jones, H. R. A., Jenkins, J. S., et al. 2012, MNRAS, submitted''). No paper announcing HD 114613 as a ''low-mass'' planet host has been published as of 2014.
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| However, that does not mean the star is not a planet host. Wittenmyer et al. (2014) found HD 114613 to show a moderate-amplitude variation in its radial velocity with a period of 10.5 years, indicative of a long-period companion.<ref name="Wittenmyer2014"/> The radial velocity semi-amplitude of 5.5 m/s translates to a planet with a minimum mass about half a Jupiter mass. The planet has an intermediate orbital eccentricity of 0.25, which means that it can be somewhat loosely considered a Jupiter analogue.
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| {{OrbitboxPlanet begin
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| | table_ref = <ref name="Wittenmyer2014"/>
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| }}
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| {{OrbitboxPlanet
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| | exoplanet = [[HD 114613 b|b]]
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| | mass = ≥0.48 ± 0.04
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| | period = 3827 ± 105
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| | semimajor = 5.16 ± 0.13
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| | eccentricity = 0.25 ± 0.08
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| }}
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| {{Orbitbox end}}
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| == Notes ==
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| {{Reflist|group=note}}
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| ==References==
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| {{reflist|refs=
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| <ref name="van Leeuwen2007">{{cite journal | url=http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL | title=Validation of the new Hipparcos reduction | last1=van Leeuwen | first1=F. | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | year=2007 | arxiv=0708.1752 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 }} </ref>
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| <ref name="Hog2000">{{cite journal | title=The Tycho-2 catalogue of the 2.5 million brightest stars | last1=Høg | first1=E. | last2=Fabricius | first2=C. | last3=Makarov | first3=V. V. | last4=Urban | first4=S. | last5=Corbin | first5=T. | last6=Wycoff | first6=G. | last7=Bastian | first7=U. | last8=Schwekendiek | first8=P. | last9=Wicenec | first9=A. | display-authors=1 | journal=Astronomy and Astrophysics | volume=355 | pages=27–30 | year=2000 | bibcode=2000A&A...355L..27H }}</ref> | |
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| <ref name="Teff">[http://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.dat A Modern Mean Stellar Color and Effective Temperatures (Teff) # Sequence for O9V-Y0V Dwarf Stars], E. Mamajek, 2011, website</ref>
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| <ref name="AbsMag">The relevant calculation for absolute magnitude is <math>\scriptstyle M = m - 5 \log_{10} \left( \frac{100}{\mathrm{parallax\ (mas)}} \right)</math>, where <math>M\!\,</math> is absolute magnitude and <math>m\!\,</math> is apparent magnitude.</ref>
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| <ref name="Takeda2007">{{cite journal | title=Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog | last1=Takeda | first1=Genya | last2=Ford | first2=Eric B. | last3=Sills | first3=Alison | last4=Rasio | first4=Frederic A. | last5=Fischer | first5=Debra A. | last6=Valenti | first6= Jeff A. | display-authors=1 | journal=The Astrophysical Journal Supplement Series | volume=168 | issue=2 | pages=297–318 | year=2007 | arxiv=astro-ph/0607235 | bibcode=2007ApJS..168..297T | doi=10.1086/509763 }}</ref>
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| <ref name=Sousa08>{{cite journal | author=Sousa, S. G. | title=Spectroscopic parameters for 451 stars in the HARPS GTO planet search program. Stellar [Fe/H] and the frequency of exo-Neptunes | journal=Astronomy and Astrophysics | volume=487 | issue=1 | year=2008 | pages=373–381 | month=August | doi=10.1051/0004-6361:200809698 | bibcode=2008A&A...487..373S | display-authors=1 | last2=Santos | first2=N. C. | last3=Mayor | first3=M. | last4=Udry | first4=S. | last5=Casagrande | first5=L. | last6=Israelian | first6=G. | last7=Pepe | first7=F. | last8=Queloz | first8=D. | last9=Monteiro | first9=M. J. P. F. G. |arxiv = 0805.4826 }}</ref>
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| <ref name="Lovis2011">{{cite journal | title=The HARPS search for southern extra-solar planets. XXXI. Magnetic activity cycles in solar-type stars: statistics and impact on precise radial velocities | last1=Lovis | first1=C. | last2=Dumusque | first2=X. | last3=Santos | first3=N. C. | last4=Bouchy | first4=F. | last5=Mayor | first5=M. | last6=Pepe | first6=F. | last7=Queloz | first7=D. | last8=Ségransan | first8=D. | last9=Udry | first9=S. | display-authors=1 | journal=Astronomy and Astrophysics (submitted) | year=2011 | arxiv=1107.5325}}</ref>
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| <ref name="Valenti2005">{{cite journal | title=Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs | last1=Valenti | first1=J. A. | last2=Fischer | first2=D. A. | journal=The Astrophysical Journal Supplement Series | volume=159 | issue=1 | pages=141–166 | year=2005 | bibcode=2005ApJS..159..141V | doi=10.1086/430500 }}</ref>
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| <ref name="Mortier2013">{{cite journal | title=On the functional form of the metallicity-giant planet correlation | last1=Mortier | first1=A. | last2=Santos | first2=N. C. | last3=Sousa | first3=S. | last4=Israelian | first4=S. | last5=Mayor | first5=M. | last6=Udry | first6=S. | display-authors=1 | journal=Astronomy & Astrophysics | volume=551 | year=2013 | arxiv=1302.1851 | bibcode=2013A&A...551A.112M | doi=10.1051/0004-6361/201220707 }}</ref>
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| <ref name="Endl2002">{{cite journal | title=The planet search program at the ESO Coudé Echelle spectrometer. III. The complete Long Camera survey results | last1=Endl | first1=M. | last2=Kürster | first2=M. | last3=Els | first3=S. | last4=Hatzes | first4=A. P. | last5=Cochran | first5=W. D. | last6=Dennerl | first6=K. | last7=Döbereiner | first7=S. | display-authors=1 | journal=Astronomy & Astrophysics | volume=392 | pages=671-690 | year=2002 | arxiv=astro-ph/0207512 | bibcode=2002A&A...392..671E | doi=10.1051/0004-6361:20020937 }}</ref>
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| <ref name="Zechmeister2013">{{cite journal | title=The planet search programme at the ESO CES and HARPS. IV. The search for Jupiter analogues around solar-like stars | last1=Zechmeister | first1=M. | last2=Kürster | first2=M. | last3=Endl | first3=M. | last4=Lo Curto | first4=G. | last5=Hartman | first5=H. | last6=Nilsson | first6=H. | last7=Henning | first7=T. | last8=Hatzes | first8=A. P. | last9=Cochran | first9=W. D. | display-authors=1 | journal=Astronomy & Astrophysics | volume=592 | year=2013 | arxiv=1211.7263 |bibcode = 2013A&A...552A..78Z | doi = 10.1051/0004-6361/201116551 }}</ref>
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| <ref name="Jones2002">{{cite journal | title=Extrasolar planets around HD 196050, HD 216437 and HD 160691 | last1=Jones | first1=Hugh R. A. | last2=Paul Butler | first2=R. | last3=Marcy | first3=Geoffrey W. | last4=Tinney | first4=Chris G. | last5=Penny | first5=Alan J. | last6=McCarthy | first6=Chris | last7=Carter | first7=Brad D. | display-authors=1 | journal=Monthly Notices of the Royal Astronomical Society | volume=337 | issue=4 | pages=1170–1178 | year=2002 | arxiv=astro-ph/0206216 | bibcode=2002MNRAS.337.1170J | doi=10.1046/j.1365-8711.2002.05787.x }}</ref>
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| <ref name="Wittenmyer2010">{{cite journal | title=The Frequency of Low-mass Exoplanets. II. The "Period Valley" | last1=Wittenmyer | first1=Robert A. | last2=O'Toole | first2=Simon J. | last3=Jones | first3=H. R. A. | last4=Tinney | first4=C. G. | last5=Butler | first5=R. P. | last6=Carter | first6=B. D. | last7=Bailey | first7=J. | display-authors=1 | journal=The Astrophysical Journal | volume=722 | issue=2 | year=2010 | arxiv=1008.5232 | bibcode=2010ApJ...722.1854W | doi=10.1088/0004-637X/722/2/1854 }}</ref>
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| <ref name="Wittenmyer2011">{{cite journal | title=The Frequency of Low-mass Exoplanets. III. Toward η<sub>⊕</sub> at Short Periods | last1=Wittenmyer | first1=Robert A. | last2=Tinney | first2=C. G. | last3=Butler | first3=R. P. | last4=O'Toole | first4=Simon J. | last5=Jones | first5=H. R. A. | last6=Carter | first6=B. D. | last7=Bailey | first7=J | last8=Horner | first8=J. | display-authors=1 | journal=The Astrophysical Journal | volume=738| issue=1 | year=2011 | arxiv=1103.4186 | bibcode=2011ApJ...738...81W | doi=10.1088/0004-637X/738/1/81 }}</ref>
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| <ref name="Howard2010">{{cite journal | title=The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters | last1=Howard | first1=Andrew A. | last2=Marcy | first2=Geoffrey W. | last3=Johnson | first3=John Asher | last4=Fischer | first4=Debra A. | last5=Wright | first5=Jason T. | last6=Isaacson | first6=Howard | last7=Valenti | first7=Jeff A. | last8=Anderson | first8=Jay | last9=Lin | first9=Doug N. C. | last10=Ida | first10=Shigeru | display-authors=1 | journal=Science | volume=330 | year=2010 | arxiv=1011.0143 | bibcode=2010Sci...330..653H | doi=10.1126/science.1194854 }}</ref>
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| <ref name="Wittenmyer2012">{{cite journal | title=The Anglo-Australian Planet Search. XXII. Two New Multi-planet Systems | last1=Wittenmyer | first1=Robert A. | last2=Horner | first2=J. | last3=Tuomi | first3=Mikko | last4=Salter | first4=G.S. | last5=Tinney | first5=C.G. | last6=Butler | first6=R.P. | last7=Jones | first7=H.R.A. | last8=O'Toole | first8=S.J. | last9=Bailey | first9=J. | last10=Carter | first10=B.D. | last11=Jenkins | first11=J.S. | last12=Zhang | first12=Z. | last13=Vogt | first13=S.S. | last14=Rivera| first14=Eugenio J. | display-authors=1 | journal=The Astrophysical Journal | volume=753 | issue=2 | year=2012 | at=169 | arxiv=1205.2765 | bibcode=2012ApJ...753..169W | doi=10.1088/0004-637X/753/2/169 }}</ref>
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| <ref name="Tuomi2013">{{cite journal | title=Signals embedded in the radial velocity noise. Periodic variations in the τ Ceti velocities | last1=Tuomi | first1=M. | last2=Jones | first2=H. R. A. | last3=Jenkins | first3=J. S. | last4=Tinney | first4=C. G. | last5=Butler | first5=R. P. | last6=Vogt | first6=S. S. | last7=Barnes | first7=J. R. | last8=Wittenmyer | first8=R. A. | last9=O'Toole | first9=S. | last10=Horner | first10=J. | last11=Bailey | first11=J. | last12=Carter | first12=B. D. | last13=Wright | first13=D. J. | last14=Salter | first14=G. S. | last15=Pinfield | first15=D. | display-authors=1 | journal=Astronomy & Astrophysics | volume=551 | year=2013 | arxiv=1212.4277 | bibcode=2013A&A...551A..79T | doi=10.1051/0004-6361/201220509 }}</ref>
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| <ref name="Wittenmyer2014">{{cite journal | title=The Anglo-Australian Planet Search. XXIII. Two New Jupiter Analogs | last1=Wittenmyer | first1=Robert A. | last2=Horner | first2=Jonathan | last3=Tinney | first3=C.G. | last4=Butler | first4=R. P. | last5=Jones | first5=H.R.A. | last6=Tuomi | first6=Mikko | last7=Salter | first7=G.S. | last8=Carter | first8=B.D. | last9=Koch | first9=F. Elliot | last10=O'Toole | first10=S.J. | last11=Bailey | first11=J. | last12=Wright | first12= D. | display-authors=1 | journal=The Astrophysical Journal | year=2014 | arxiv=1401.5525 }}</ref>
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| }}
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| {{Nearest star systems|14}}
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| {{Stars of Centaurus}}
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| [[Category:Centaurus (constellation)]]
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| [[Category:Henry Draper Catalogue objects|114613]]
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| [[Category:Hipparcos objects|064408]]
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| [[Category:HR objects|4979]]
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| [[Category:Gliese and GJ objects|0501.2]]
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| [[Category:G-type subgiants]]
| |
There's no incertitude that Google is comely a full-mature hardware company, merely the up-to-the-minute Google X cast is a stack dissimilar that tablets and smartphones ??�the companion hardly announced that it's edifice a "smart contact lens." However, it's non meant to be a miniaturized variant of Chalk ?? it's meant to aid diabetes patients sustenance cross of their glucose levels. Interior the genus Lens is a miniaturized radio receiver chip off and glucose monitor that leave mensurate the glucose levels of the wearer's tears.
Google's hoping that it'll be a less terrible and encroaching way of life to monitor lizard glucose levels than the distinctive method acting of pricking a digit and examination pedigree droplets multiple multiplication a sidereal day. Ideally, the detector would be able-bodied to sire a version one time per second, and Google wants it to roleplay as an early word of advice device for when glucose levels kickoff dropping ?? the troupe imagines putt a small LED illuminate in the crystalline lens that could argue levels dropping supra or down the stairs a prepare doorstep.
It's not a New idea for co-Divine Babek Parviz ?? backrest in 2009,�Parviz showed Wired a connected inter-group communication electron lens meant to measuring vital signs. And piece this is fresh run aground for Google, the estimate of a attached meet genus Lens for specifically measure glucose levels isn't Modern ?? Microsoft and the University of Washington�worked on a standardized contrive rearward in 2011. Both Parviz and gent co-fall flat Brian Elisha Graves Otis were at the University of Washington and contributed to that project, as intimately.
Of course, this send off is hush a estimable ways polish off from existence a realness ?? Google says its operative with the Food and Drug Administration and is also looking for for early partners World Health Organization are "experts in bringing products like this to market." The company wants partners to apply its technology to grow these lenses and as well establish apps to shuffling the measurements useable to users. There's no Word of God on when this lense mightiness be a reality, or even if it'll sour as planned, only it's sound to project Google victimization its technology art to examine and work a long-standing aesculapian trouble.
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