Unconfirmed/Unpublished Planets Catalogue

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by marasama on 5th January 2010, 2:40 pm

Epsilon Aurigae solved?
According to this page
http://www.hposoft.com/Campaign09.html
The hypothesis has ran with eclipsing binary B stars or 2 gas giant planets.

Have not found any papers on this.

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Lazarus on 5th January 2010, 5:10 pm

Regarding Epsilon Aurigae, there's a Spitzer press release out today:

Centuries-Old Star Mystery Coming to a Close

Spitzer measurements favour the low-mass model for the system, making it a little less extreme.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 7th January 2010, 5:27 pm

Pulsar planet or what else??

Discovery of short-period binary millisecond pulsars in four globular clusters

We report the discovery, using the Parkes radio telescope, of binary millisecond pulsars in four clusters for which no associated pulsars were previously known. The four pulsars have pulse periods lying between 3 and 6 ms. All are in circular orbits with low-mass companions and have orbital periods of a few days or less. One is in a 1.7 hr orbit with a companion of planetary mass. Another is eclipsed by a wind from its companion for 40% of the binary period despite being in a relatively wide orbit. These discoveries result from the use of improved technologies and prove that many millisecond pulsars remain to be found in globular clusters.

PSR J1807-24 in NGC 6544 globular cluster.

Authors think it is a brown dwarf or a massive planet. Not a hydrogen or helium dwarf.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Lazarus on 16th January 2010, 10:30 am

So despite being in close orbit around a pulsar there appears to be no evidence for material being blasted off the object? Weird. As noted, might be a near-face-on system.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 8th April 2010, 4:30 am

Some cool unpublished(?) news:

1) 61 Cygni revamped? No fulltext, though.

Orbit and estimations of masses of components of ADS 14636 (61 Cygni) on the basis of photographic observations at Pulkovo Observatory

The investigation of the wide double star 61 Cyg fulfilled by means of long-term series (40 years) of photographic observations of 26" refractor of Pulkovo observatory. The purposes of the investigation are 1) determination of the pair's orbit and masses of its components and 2) detection of possible invisible satellites. The two more long-term series of wide double stars - ADS 7251 (38 yr.) and ADS 14710 (23 yr.) were used for control. Obtained photo-plates were measured by means of automatic measurement machine "Fantazia" in Pulkovo observatory. Relative positions (distances between components and positional angles) were calculated for all pairs. The relative orbit of 61 Cyg was constructed and total mass of the pair was calculated by means of the Apparent Motion Parameters Method developed in Pulkovo observatory. These series were investigated by means of Scargle's and CLEAN methods to detect periodic deviations in orbital motion. Far star ADS 14710 (pi=0.0016) was used as control star. Two peaks were detected in periodogram of X projection of components relative motion of 61 Cyg only. They correspond to periods of 6.4 and 11.2 years. The investigation of separate motion of each component of 61 Cyg relative to surrounded stars fulfilled. The mass ratios and hence individual masses of its components calculated. They are 0.74 0.13 and 0.46 0.07 of solar masses for primary and secondary components respectively. There is a small peak on periodogram of X projection of separate motion of 61 Cyg A. It corresponds to period of 6.2 years. We suppose that invisible satellites may be in 61 Cyg's system, but their mass does not exceed 0.01 solar mass.

2) Back in 2007 very low-mass companions to young stars in Taurus-Auriga at wide separations. Excluding brown dwarfs (0.02-0.07 Solar masses) here I show you those with companion around or below 0.01 Solar masses (=10 Jupiter masses)!

The Role of Mass and Environment in Multiple Star Formation: A 2MASS Survey of Wide Multiplicity in Three Young Associations

- ScoPMS 8a - M4V+M9V, 0.24+0.01 Mso, 229 AUs
- V410 X-ray 5 - M5.5V+M9V, 0.14+0.01 Mso, 1924 AUs
- LkCa 4 (V1068 Tau) - K7V+M9V, 0.72+0.01 Mso, 1285 AUs
- RX 1539.4-3446 B* - K7V+L0V?, 0.77+<0.01 Mso, 4259 AUs

(*)= Seems a highly multiple system, at least quintuple or sextuple.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 14th May 2010, 4:06 am

Discovery of a cataclysmic variable with a sub-stellar companion

We find that the ROSAT source 1RXS J105010.3-140431 is a cataclysmic variable with orbital period of 88.6 min and a spectrum closely resembling WZ Sge. In particular, emission lines are flanked by Stark-broadened absorption wings probably originating in the photosphere of a compact object. The Balmer absorption lines can be modeled by the spectrum of a DA white dwarf with 13 000 < T_eff < 24 000 K. The strong absorption lines allowed us to obtain direct radial velocities of the white dwarf using the cross-correlation technique. We find an extremely low white dwarf radial velocity half amplitude, K_wd = 4 +/- 1 km s-1. This is consistent with the upper limit obtained from the Hα emission line wing K < 20 km s-1. The corresponding mass function is incompatible with a main sequence secondary, but is compatible with a post orbital period minimum cataclysmic variable with a brown dwarf-like secondary. The formal solution gives a secondary mass of 10-20 Jovian masses. Doppler maps for the emission lines and the hypothesis of black-body emission indicate a steady state (T ~ r-3/4) accretion disk mainly emitting in Hα and an optically thicker hotspot with a strong contribution to the higher order Balmer lines and He I 5875. As in other long cycle length dwarf novae, evidence for inner disk removal is found from the analysis of the emission lines.

Since 2001.
Unlikely a He dwarf, brown dwarf or superplanet forming CV system?
No updates so far, I think.

Star lies in Hydra.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 16th May 2010, 6:22 am

This is funny to read, it is from 1997.

Astrometric Indications of Brown Dwarfs based on HIPPARCOS Data

According to the author two well known M dwarfs (hosting low-mass planets) had to host instead brown dwarf companions in wider orbits.

For instance Gj 176 has a 70 Mj companion with 463.8 days orbital period. Same for Gliese 433, with a 30 Mj with 523 days period.

Both the stars actually show NO substellar companions more massive than 10 Mj. Rather they have superearths in close orbits.

Wondering how such candidates would have been detected...
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Sirius_Alpha on 16th May 2010, 6:52 am

Most likely the Hipparcos results were spurrious.

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 16th May 2010, 7:55 am

Due to the 3s-effects I asked for a confrmation ofthis result: the 2D IR speckle interferometer observation sat ESO SHARP on the NTT (Leinert &Woitas,MPIA Heidelberg, private communication 1997) confirms that Gliese 433 has a very faint companion!

Very, very, very, very, very faint...

Quite not a brown dwarf. Scroll down...
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Sirius_Alpha on 16th May 2010, 8:41 am

Interesting. According to the paper, both interferrometry and Hipparcos astrometry agree on the presence of a companion. I eagerly await the paper describing the discovery of Gliese 433 b...

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 16th May 2010, 1:38 pm

Yes, I agree, as well for GJ 667 C. No paper since October 2009.
Quite a long wait, so far.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 24th May 2010, 6:07 am

Read carefully

The Phenomenon of Double Star 61 Cygni: Some Hypothesis on Its Satellites pg. 159

One of the most satisfactory models yields the following elements: P=6.4 yrs, a=0''.019, e=0.55, i=54[...] and the low limit of the mass of possible satellite is 0.014 Mso

Unburying 61 Cygni C in 2007? And again a brown dwarf.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Sirius_Alpha on 6th July 2010, 9:17 am

Does anyone know what happened to this?

Dynamical Masses and Third Bodies in the Sirius System
http://adsabs.harvard.edu/abs/2007hst..prop11290B

Abstract wrote:...At present, there is a tantalizing suggestion in our data that there indeed may exist a substellar or planetary third body in the system...

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Lazarus on 6th July 2010, 1:31 pm

Sirius would definitely be an interesting system to find planets in: for a start the binary ought to have been more compact before Sirius B lost most of its mass. The system might therefore be a good place to go hunting for second-generation planets produced from material ejected by Sirius B during its giant stage.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by ciceron on 6th July 2010, 2:28 pm

Or a stripped down jovian , bereft of its outer atmospheric layers after the event.

Coincidentally today was re-reading an old article about sirius system being red in historic times. Does anyone knows if that is proven or otherwise ? There were references about the red colour of the star by Seneca in the 1st Century and Ptolomeus in the 2nd Century , and a less reliable reference by Gregory of Tours in the 6th Century.

I wonder if the remains of the Sirius B ejecta may be dragging the system and cause the measured perturbations. In that case , some kind of flourescence should be observed.

Just wondering , i haven't read anything recent on the sirus system.



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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 19th October 2010, 4:20 pm

"Tantalizing" is the right word

Sirius B is the nearest and brightest of all white dwarfs WDs, but it is fiendishly difficult to observe from the ground because of the overwhelming brightness of Sirius A. We propose a continuation of our program of imaging observations of the Sirius system with WFPC2, which has been underway since 2001. The resulting astrometric data will not only greatly improve the precision of the binary orbit and the dynamical mass measurements for both the main-sequence and WD components, but will also test definitively for the claimed presence of a third body in this famous system, down to planetary masses. At present, there is a tantalizing suggestion in our data that there indeed may exist a substellar or planetary third body in the system. Our team has also obtained superb spectra of Sirius B using STIS, and we have achieved an excellent fit to the spectrum using model stellar atmospheres. However, the implied mass of the WD disagrees significantly with the dynamical mass implied by the existing visual-binary orbit which still has to be based on a combination of low-accuracy ground-based astrometry plus the small number of existing HST astrometric observations. This is another critical motivation for improving the astrometry
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 25th November 2010, 7:21 am

Even stronger evidence of planet around HMW 15 (V713 Persei)

The Light Curve of V713 Per (HMW 15): Evidence for Gravitational Sculpting by an Object Embedded in the Circumstellar Disk

HMW 15 (V713 Per, H 187, TJ 108, LRLL 35) is a G-type weak-line T Tauri star (WTTS) in the extremely young cluster IC 348. It has an age of about 3 My, a mass of about 1.5 solar mass and a distance of 300 pc. What distinguishes it from other WTTS is a cyclic variation in optical brightness with an amplitude of about 0.8 mag and a period of 1717 d or 4.7 yr (Nordhagen et al. 2006, ApJ 646, 151). The star shows no detectable radial velocity variations to stringent limits (Grinin et al. 2008, A&A 489,1233) indicating that the periodicity is not caused by a stellar companion. Two complete cycles of this variation have now been observed and we present and discuss its form and features. We suggest that the main cause of the periodic variation is a massive embedded planet or protoplanet orbiting at a distance of 3.3 AU from the central (single) star. Other features in the light curve can be seen at the Lagrangian points (L3, L4 and L5) of this system, where we suppose that gravitational sculpting by the planet has been active. Continued monitoring of this unique and potentially important system is obviously warranted and is needed to test our hypothesis. We thank the NASA-Origins program for its support of this work through a grant to WH and the NSF/REU program for supporting the participation of one us (AY)
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 26th November 2010, 7:11 am

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Lazarus on 26th November 2010, 1:45 pm

Less than 3 stellar radii at periastron! Looks a bit like a smaller version of the Iota Draconis planet.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Sirius_Alpha on 27th November 2010, 9:13 am

Regarding V713 Persei, why are the changes in brightness not being attributed to the star itself? i.e. why is a planet a better explanation than intrinsic stellar variability?

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 10th December 2010, 5:59 am

A planet around ER Vulpeculae?

http://www.springerlink.com/content/mk3617475k58x47l/fulltext.pdf

we obtain: a sin(i) = 0:026 a.u. f(m) = 1:88e-08M . Using i = 67 we found that the mass of the third body and the orbital dimensions are M3 =0.0048MSo and a = 0.028 a.u. respectively. Considering that the distance is 46 pc,these figures correspond to angular distance between the third body and the eclipsing pair of 0.000003 respectively. It is very difficult to detect the supposed thirdbody because its luminosity is very extremely small.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Lazarus on 20th December 2010, 1:27 pm

Aldebaran b has appeared in the EPE unconfirmed catalogue. Reason for unconfirmed status is given as lack of publication in a refereed journal.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 20th December 2010, 4:19 pm

Lazarus wrote:Aldebaran b has appeared in the EPE unconfirmed catalogue. Reason for unconfirmed status is given as lack of publication in a refereed journal.

Same for Arcturus.
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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Lazarus on 25th January 2011, 3:07 am

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Re: Unconfirmed/Unpublished Planets Catalogue

Post by Edasich on 25th January 2011, 5:11 am


Nice. However Sirius A seems hiding an elusive companion.
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Re: Unconfirmed/Unpublished Planets Catalogue

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