 v sin i from Pasquini & Pallavicini (1991) lead to a radius of 1.06R⊙ at i close to 90 •.
The star was also target for the search of a debris disc (Greaves et al. 2004) but no disc could be detected at 850 µm with a flux limit of 2σ (2 mJy) corresponding to a total of 0.02 M⊙ of dust per star.
The FOCES spectra were observed on Dec 01 2001 with a signal-to-noise ratio of 250. We measure a lithium EW of 72.5 mÅ which transforms to a lithium abundance of log N (Li) = 2.30, and the core of Hα is filled-in to a level of 5%. Also the cores of calcium H&K-lines are filled. All in all the star is quite active. The magnetically sensitive iron line at 6173Å is asymmetric which lead to the conclusion that there is a strong magnetic field on the surface. Our spectral synthesis leads to the stellar parameters listed in Tab. 1. The difference between the predicted spectroscopic distance and the parallax measurement of Hipparcos (Hipparcos, ESA 1997) is only 2.8%. Gaidos et al. (2000) have measured a rotation period of 7.81 ± 0.01 days. Using our estimate of the radius and the v sin i = 6.39 km s −1 we estimate an inclination of 0.054 • and v = 6675 m s −1.

HIP 18512, [GKL99] 104, HD 24916 A
Relying on kinematic data, Madsen et al. (2002) and Montes et al. (2001) list HIP 18512 as a member of the Ursa Major association. They estimate a parallax π = 63.3 ± 2.0 mas and measured by Hipparcos of π = 63.41 ± 2.0 mas, respectively. Favata et al. (1997) estimated a temperature of T eff = 4394 K and they measured lithium equivalent width of W (Li) = 4 mÅ and an abundance of log N (Li) = −0.55. They consider the star kinematically young.
The results of our analysis of the FOCES spectra observed Dec 01 2001 and with a SNR of 300 give the parameters: T eff ∼ 4600 ± 100, [F e/H] = 0.03 ± 0.07, log g = 4.60 ± 0.10. We do not detect a trace of the lithium absorption line at 6707Å.

HIP 26779, [GKL99] 145, HD 37394
The space motion derived by (Gaidos 1998) show that the star is a member of the local association. The stellar parameters they derive are T eff = 5200 K, W (Li) = 1.3 ± 3.2 mÅ which lead to a lithium abundance of log N (Li) = 0.03±0.03, v sin i = 4.0 km s −1 and an inclination range i = 45 • − 90 •. Analysing the FOCES spectra, we get a very good agreement of the spectroscopic distance with the Hipparcos distance of only 0.5%.

EK Dra, HIP 71631, HD 129333, [GKL99] 306
EK Dra is an interesting young binary where it is possible to solve the Keplerian orbit and derive the true masses König et al. (2005). The masses of the two stars are 0.90 ± 0.10 M⊙ and 0.50 ± 0.10 M⊙, respectively.
We also performed a spectral synthesis analysis in course of that publication. The results are summarised in Tab. 1. As mentioned in König et al. (2005), EK Dra has a large overabundance. The measured lithium equivalent width in the observed spectrum is 190 ± 10 mÅ. Modelling the lithium line this leads to a lithium contents of log N (Li) = 3.30 ± 0.05.

HIP 73555, [GKL99] 312, HD 133208
The recent classification in the SIMBAD database list it as G8IIIa which would mean that it is a post-main-sequence subgiant. Since the star was listed in the catalogue it was observed with high resolution spectroscopy using the FO-CES instrument at Calar Alto in Feb. 13th 2001.
The spectral synthesis analysis reveal the nature of the star as a subgiant given the estimated log g using the Fe I/Fe II and Fe/Mg ionisation equilibrium.
Placing the star into an Herzsprung-Russell diagram (see Fig. 1) using post-main-sequence tracks of Schaller et al. (1992) we estimate the mass of 3.4 ± 0.2 M⊙ and an age of 240 Myrs. This would imply that it is still a young star, but because of its higher mass the evolution time scales are smaller and yet it has reached the postmain-sequence. Calculating a spectroscopic parallax and comparing it with the Hipparcos parallax the difference is 3.6%. The kinematics of this star reveal a space velocity of (U/V /W ) = (6.6/ − 17.1/ − 1.2) km s −1. This is consistent with the Pleiades, α Per, IC 2602, and Coma Berenice Table 1. Spectral parameters of the flare-stars derived by spectral synthesis analysis. log(L X /L bol ) is a measure for the activity of the stars.  moving groups, which are summarised as the local association. Since the local association is a conglomerate of comoving groups with different ages, the age estimated from the post-main-sequence tracks of Schaller et al. (1992) cannot be confirmed or disproved.
For the subgiant HIP 73555 radius measurement are available and listed in Richichi & Percheron (2002) and references therein. By interferometry they measure a diameter of 2.99 ± 0.01 mas with a parallax of π = 14.91 ± 0.57 mas this leads to a diameter of D = 43.0 ± 2.0 R⊙, or radius R = 21.5 ± 1.0 R⊙. Our measured temperature can be used to predict a radius: 18.5 ± 0.5 R⊙. The radius predictions are in agreement, so we are confident that our measured effective temperature is reasonable.  Table 3. Spectral parameters of HIP 73555 derived using the spectral synthesis analysis methods described before (first row of the table). The last three rows summarise the work of the other authors. The spectral parameters were used to calculate the spectroscopic distance and compare to the Hipparcos distance to investigate the accuracy of the analysis.

Reference
T  William (1990), B&G: Bell & Gustafsson (1989) level namely the line-filling would support an age of 100-300 Myrs. Chen et al. (2001)  The spectral syntheses analysis reveals a star close to the main-sequence on the zero-age main-sequence (ZAMS). The measured lithium equivalent width in the observed spectrum is 100.8 ± 0.8 mÅ. Modelling the lithium line this leads to a lithium contents of log N (Li) = +2.81 ± 0.09. Thus, like EK Dra, HN Peg also has a large overabundance of lithium. The stellar parameters are listed in Tab. 1.

HIP 114385, HD 218739 and HIP 114379, [GKL99] 440, HD 218738
The stars HIP 114385 and HIP 114379 A&B form a triple system where HIP 114385 and HIP 114379 from a visible binary system and HIP 114379 A&B is a spectroscopic and adaptiv optics (AO) binary. HIP 114385 and HIP 114379 are located at the same distance at 34.06 ± 2.31 mas and 39.56 ± 7.67 mas respectively. They are comoving. Note the big error in the parallax measurement of Hipparcos. For HIP 114379 this clearly shows that the companion disturbed the precision of the parallax measurement. But also the stray light from HIP 114379 (π = 39.56 ± 7.67 mas) disturbed the parallax measurement of HIP 114385 (π = 34.06 ± 2.31 mas) which can be noticed by the relative big error. For HIP 114379 the following data is available from the catalogue of nearby star metallicities (Zakhozhaj & Shaparenko 1996) obtained from photometric UBV data (π = 28.7 mas, [F e/H] = −0.30). This result must be regarded with care because the star is a binary and the data has not been corrected for this.
For the visual companion (HIP 114385) no data from that catalogue is available. We measure the metallicity of the companion star to be [F e/H] = 0.08 ± 0.07, much higher than its companion. It is not clear, why the companion should have a different metallicity. We can only guess that the metallicity determined by photometry is not correct.
Its lithium is already burned which makes the star older than the Pleiades, but its activity indicate an age similar to the Ursa Major cluster.

Distance determination
Using the stellar parameter we derive a spectroscopic distance which we compare to the parallax measurements of Hipparcos. As