Peripheral Members of M67

Platais, I.; Kozhurina-Platais, V.; Geffert, M.; Frolov, V. N.

doi:10.1007/978-94-011-0125-7_73

Cited by 6 publications

(27 citation statements)

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“…The presence of a bright progenitor of V445 Pup having a visual magnitude of 13.1 was first noted by Platais et al (2001). Its absolute proper motion was small, µ = 0.…”

Section: Introductionmentioning

confidence: 93%

The progenitor and remnant of the helium nova V445 Puppis

Goranskij,

Shugarov,

Zharova

et al. 2010

Preprint

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“…The presence of a bright progenitor of V445 Pup having a visual magnitude of 13.1 was first noted by Platais et al (2001). Its absolute proper motion was small, µ = 0.…”

Section: Introductionmentioning

confidence: 93%

The progenitor and remnant of the helium nova V445 Puppis

Goranskij,

Shugarov,

Zharova

et al. 2010

Preprint

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“…We used the Southern Proper Motion (SPM) program plates (Platais et al 1995;Girard et al 1998) to derive proper motions of potential TWA members. The SPM plates contain multiple images of bright stars in the TWA region, with a mean epoch difference ranging from 20 to 25 years.…”

Section: Observationsmentioning

confidence: 99%

Discovery of Seven T Tauri Stars and a Brown Dwarf Candidatein the Nearby TW Hydrae Association

Webb

Zuckerman

Platais

et al. 1999

The Astrophysical Journal

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373

490

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We report the discovery of five T Tauri star systems, two of which are resolved binaries, in the vicinity of the nearest known region of recent star formation, the TW Hydrae Association. The newly discovered systems display the same signatures of youth (namely high X-ray flux, large Li abundance and strong chromospheric activity) and the same proper motion as the original five members. These similarities firmly establish the group as a bona fide T Tauri association, unique in its proximity to Earth and its complete isolation from any known molecular clouds.At an age of ∼10 Myr and a distance of ∼50 pc, the association members are excellent candidates for future studies of circumstellar disk dissipation and the formation of brown dwarfs and planets. Indeed, as an example, our speckle imaging revealed a faint, very likely companion 2 ′′ north of CoD-33 • 7795 (TWA 5). Its color and brightness suggest a spectral type ∼M8.5 which, at an age of ∼10 7 years, implies a mass ∼ 20 M Jupiter .

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“…Firstly, the outburst amplitude, which, according to our estimate (Table 21) is about 12 , should be counted from the brightness of the post-nova, which in 2009 had a brightness of V≈19 . Otherwise, according to the brightness of the pre-nova, B=14.3 (Goranskij et al, 2010) or m =13.1 (Platais et al, 2001) we have an amplitude should be much lower (not higher than 5.9 ). Secondly, a very long and deep light minimum on 10 , which according to the moment of the beginning of the brightness drop corresponds to the D4 V1280 Sco type.…”

Section: Novae With Unique Light Curvesmentioning

confidence: 79%

Review of light curves of novae in the modified scales. II. Classical novae

Rosenbush¹

2020

Preprint

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The presentation of the light curves of the novae on the logarithmic scale of the radius of the shell ejected during the outburst and in the scale of the amplitude of the outburst simplified the review of the light curves of all the known, about 500, classical novae of our Galaxy and the Large and Small Magellanic Clouds. As a result, the modified light curves about of 250 classical novae were grouped into 7 typical groups with subgroups defined by the light curves of prototypes.The largest group is the DQ Her group with V1280 Sco as the main prototype and the key to grouping. Novae of this group have three or four variants of a dust condensation. Novae of the small GQ Mus group may be a bright X-ray source during an outburst. CP Pup, CP Lac, V1974 Cyg, and V1493 Aql are prototypes for 4 groups with close tilts of the initial brightness decline phase of the light curves. The group with the prototype RR Pic, including the HR Del subgroup, has a prolonged state of maximal brightness with the presence of several brightness variations before the final decline phase.The relationship of groups of novae, or form of the light curve, with processes in the circumstellar and circum-binary system environment is discussed. The material ejected during an outburst forms expanding shells of a generally ellipsoidal shape. In the Lac, Pup, and Cyg groups, the shells do not show a pronounced regular structure, except for their ellipsoidal shape. Shells of novae with a dust condensation (the DQ Her group) have an ellipsoidal shape with an equatorial belt. The unique shell of CK Vul, Nova Vul 1670, gives an idea about the possible shape of the shells of other members in the V1493 Sql group. The prototypes RR Pic and HR Del have a very bright belt. Each of groups has own position along the well-known "absolute maximal magnitude, rate of brightness decline" relation.

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Peripheral Members of M67

Cited by 6 publications

References 0 publications

The progenitor and remnant of the helium nova V445 Puppis

The progenitor and remnant of the helium nova V445 Puppis

Discovery of Seven T Tauri Stars and a Brown Dwarf Candidatein the Nearby TW Hydrae Association

Review of light curves of novae in the modified scales. II. Classical novae

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