Evolutionary tracks and isochrones for 
low- and intermediate-mass stars: From 0.15 to 7 $M_{\odot}$, 
and from $Z=0.0004$ to 0.03

Girardi, L.; Bressan, A.; Bertelli, G.; Chiosi, C.

doi:10.1051/aas:2000126

Cited by 2,179 publications

(911 citation statements)

References 32 publications

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“…The solid line shows the M V magnitude per solar mass for solar metallicity and a Salpeter (1955) MF with a lower mass limit of 0.1M ⊙ from Bruzual & Charlot (2003). The other curves show our calculations for Salpeter MFs with lower mass limits of 0.01M ⊙ , 0.1M ⊙ and 1.0M ⊙ (long-dashed, dotted-dashed and triple dotted-dashed lines) and a Kroupa (2002) MF (short-dashed line), obtained by populating solar-metallicity isochrones from Girardi (2000) according to the various MFs. It is not strictly correct to put all YMCs on the same plot, since the clusters in NGC 4214 and NGC 4449 may have metallicities of only 1/4-1/3 solar .…”

Section: Virial Mass-to-light Ratios and The Mfmentioning

confidence: 86%

Young Massive Clusters in Non-Interacting Galaxies

et al. 2005

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Section: Virial Mass-to-light Ratios and The Mfmentioning

confidence: 86%

Young Massive Clusters in Non-Interacting Galaxies

et al. 2005

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“…HD 59686 A is a slightly metal-rich star with [Fe/H]=0.15 ± 0.1 dex (Hekker & Meléndez 2007). To derive the stellar mass, we interpolated between the evolutionary tracks (Girardi et al 2000), stellar isochrones, and metallicities using a trilinear interpolation scheme. This approach commonly allows two possible solutions depending on the evolutionary status of the star, namely red giant branch (RGB) or horizontal branch (HB).…”

Section: Stellar Propertiesmentioning

confidence: 99%

Precise radial velocities of giant stars

Ortiz

Reffert

Trifonov

et al. 2016

A&A

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Context. For over 12 yr, we have carried out a precise radial velocity (RV) survey of a sample of 373 G-and K-giant stars using the Hamilton Échelle Spectrograph at the Lick Observatory. There are, among others, a number of multiple planetary systems in our sample as well as several planetary candidates in stellar binaries. Aims. We aim at detecting and characterizing substellar and stellar companions to the giant star HD 59686 A (HR 2877, HIP 36616). Methods. We obtained high-precision RV measurements of the star HD 59686 A. By fitting a Keplerian model to the periodic changes in the RVs, we can assess the nature of companions in the system. To distinguish between RV variations that are due to non-radial pulsation or stellar spots, we used infrared RVs taken with the CRIRES spectrograph at the Very Large Telescope. Additionally, to characterize the system in more detail, we obtained high-resolution images with LMIRCam at the Large Binocular Telescope. Results. We report the probable discovery of a giant planet with a mass of m p sin i = 6.92 +0.18 −0.24 M Jup orbiting at a p = 1.0860 +0.0006 −0.0007 au from the giant star HD 59686 A. In addition to the planetary signal, we discovered an eccentric (e B = 0.729 +0.004 −0.003 ) binary companion with a mass of m B sin i = 0.5296 +0.0011 −0.0008 M orbiting at a close separation from the giant primary with a semi-major axis of a B = 13.56 +0.18 −0.14 au. Conclusions. The existence of the planet HD 59686 Ab in a tight eccentric binary system severely challenges standard giant planet formation theories and requires substantial improvements to such theories in tight binaries. Otherwise, alternative planet formation scenarios such as second-generation planets or dynamical interactions in an early phase of the system's lifetime need to be seriously considered to better understand the origin of this enigmatic planet.

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“…The B − V colors are ours, whereas the V − I colors are taken from Sung et al (1999) and available only for stars brighter than V 16.7. We overplot the color-reddened 230-Myr isochrone derived from Girardi et al (2000) and corresponding to the cluster parameters taken from Sung et al (1999).…”

Section: Candidate Member Selectionmentioning

confidence: 99%

RACE-OC project: rotation and variability in the open cluster M 11 (NGC 6705)

Messina

Parihar

Koo

et al. 2010

A&A

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Context. Rotation and magnetic activity are intimately linked in main-sequence stars of G or later spectral types. The presence and level of magnetic activity depend on stellar rotation, and rotation itself is strongly influenced by the strength and topology of the magnetic fields. Open clusters represent especially useful targets for investigating the connection among rotation, activity, and age. Over time, stellar activity and rotation evolve, providing us with a promising diagnostic tool to determine the age of the field stars.Aims. The open cluster M11 has been studied as a part of the RACE-OC project (Rotation and ACtivity Evolution in Open Clusters), which aims to explore the evolution of rotation and magnetic activity in the late-type members of open clusters with different ages. Methods. Photometric observations of the open cluster M 11 were carried out in June 2004 using the LOAO 1 m telescope. The rotation periods of the cluster members were determined by Fourier analysis of photometric data time series. We investigated the relations between the surface activity, characterized by the light curve amplitude, and rotation. Results. We have discovered a total of 75 periodic variables in the M 11 FoV, of which 38 are candidate cluster members. Specifically, among cluster members we discovered 6 early-type periodic variables, 2 eclipsing binaries, and 30 bona-fide single periodic late-type variables. Considering the rotation periods of 16 G-type members of the almost coeval 200-Myr M 34 cluster, we could determine the rotation period distribution from a more numerous sample of 46 single G stars at an age of about 200-230 Myr and determine a median rotation period of P = 4.8 d. Conclusions. A comparison with the younger M 35 cluster (∼150 Myr) and with the older M37 cluster (∼550 Myr) shows that G stars rotate more slowly than younger M 35 stars and more rapidly than older M 37 stars. The measured variation in the median rotation period is consistent with the scenario of rotational braking of main-sequence spotted stars as they age. Finally, G-type M11 members have a level of photospheric magnetic activity, as measured by light curve amplitude, comparable to what is observed in the younger 110-Myr Pleiades stars of similar mass and rotation.

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Evolutionary tracks and isochrones for low- and intermediate-mass stars: From 0.15 to 7 $M_{\odot}$, and from $Z=0.0004$ to 0.03

Cited by 2,179 publications

References 32 publications

Young Massive Clusters in Non-Interacting Galaxies

Young Massive Clusters in Non-Interacting Galaxies

Precise radial velocities of giant stars

RACE-OC project: rotation and variability in the open cluster M 11 (NGC 6705)

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