Upcoming new (young) planet?

Happy new year from Edasich! And here for you tasty news, though no full text available so far.

Detection of the Youngest Known Exoplanet

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Since 2004, we have been conducting a visible light radial velocity survey at McDonald Observatory of the Taurus-Auriga low-mass star forming region. Our goals are to detect young, giant planets in order to identify the timescale for planet formation, and to search for young brown dwarfs in order to explore whether the brown dwarf desert is the result of formation or evolution. Since it has been shown that bisector analysis is not always adequate to rule out star spot induced radial velocity signals, we conduct follow-up K band observations at the IRTF to distinguish true companions from stellar activity. As part of our ongoing survey, we present the first positive detection of a short-period, giant planet around a 1-2 Myr old classical T Tauri star. Our data suggest a planet mass of 6 Mjup and an orbital solution with P = 8.28 days, a = 0.069 AU, and e = 0.53. While we find considerable uncertainty in some of our orbital parameters (notably e), infrared observations scheduled for late Fall 2009 should improve the precision of the planet's orbital elements. We also present preliminary results from other promising candidates in our survey.

Maybe DN Tauri? Since this star showed similar periodicity to disentangle from stellar activity and putative companion mass down to

A Young Planet Search in Visible and IR Light: DN Tau, V836 Tau, and V827 Tau

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For DN Tau we found P=6.33±0.20 days and a false alarm probability (FAP) of 0.001

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Initial analysis of 20 visible light RVsfor DN Tau, taken over 2.5 years, indicated convincingmodulation with P=7.5 days and FAP=0.002. Althoughnot markedly different from rotation period estimates of6.0−6.4 days (Bouvier et al. 1993; Percy et al. 2006), 2for P=7.5 days was more favorable than that for a secondarypeak at 6.3 days.

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These results indicate that no planets are presentaround DN Tau or V836 Tau with masses greater than afew MJup at <0.5 AU or 10 MJup at 1 AU, despite theabsence of a correlation between the visible light RVs and bisector spans.

I hope this could not turn out an embargo breach. Mine are just speculations.

Dynamics of Cats also mentions this one.

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Or the theory for giant planet formation is wrong, still, which is inconceivable.

Heh heh heh.

These bizarre young exoplanets use to play hide and seek.