A Study of the B Stars in the Orion Belt Region.

Hardie, R. H.; Heiser, A. M.; Tolbert, C. R.

doi:10.1086/148052

Cited by 14 publications

(16 citation statements)

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“…This catalogue, which will be completed shortly, provides for the first time combined information about the variability and the moltiplicity of all the stars with a visual magnitude less than 5. Note that the magnitude of the three stars of the Belt are in good agreement with those reported in the work by Hardie, Heiser, & Tolbert (1964) which is the most recent peer-reviewed paper on the subject. Table 1.…”

Section: Comparison Between the Dimensions Of The Giza Pyramids And Tsupporting

confidence: 87%

Archaeoastronomical Study of the Main Pyramids of Giza, Egypt: Possible Correlations with the Stars?

Orofino¹,

Bernardini²

2016

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Since long time various qualitative speculations have been proposed about the link between the three major Giza pyramids and the stars. In particular, according to a popular and controversial hypothesis (the so-called Orion Correlation Theory), a perfect coincidence would exist between the mutual positions of the three stars of the Orion Belt and those of the main Giza pyramids. In the present paper, this apparent coincidence has been subjected to some statistical verifications, in order to assess the probability that the correlation between stars and pyramids, both in relative position and in luminosity/height, can be merely due to the case. These statistical analyses have been performed by means of Monte Carlo simulations and have been coupled with previous astronomical/astrophysical tests of the presumed correlation, finding that the coincidence does not seem to be fortuitous and that it is compatible with the naked-eye astrometry and photometry of the Orion Belt stars. On the contrary, unlike what stated by another popular and controversial theory (the so-called Cygnus-Giza Correlation), we have found no coincidence between the mutual positions of the three pyramids and those of the three stars of the short arm of the asterism of Northern Cross, in the Cygnus constellation.

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Section: Comparison Between the Dimensions Of The Giza Pyramids And Tsupporting

confidence: 87%

Archaeoastronomical Study of the Main Pyramids of Giza, Egypt: Possible Correlations with the Stars?

Orofino¹,

Bernardini²

2016

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“…9. V-band magnitudes of HD 37806 from the literature (Hardie et al 1964;Warren & Hesser 1977;de Winter et al 2001, see Sect. 2.1; crosses), ESO (Manfroid et al 1991, see Sect.…”

Section: Discussion and Interpretationmentioning

confidence: 99%

“…HD 37806 was observed in the Johnson V and Strömgren y (transformed to V) bands in 1959-1962and 1968by Hardie et al (1964 and Warren & Hesser (1977). Additionally, de Winter et al (2001) observed the star in 1986 and 1992.…”

Section: Archival Datamentioning

confidence: 98%

Photometric variability of the Herbig Ae star HD 37806

Ruciński

Zwintz

Hareter

et al. 2010

A&A

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Context. The more massive counterparts of T Tauri stars, the Herbig Ae/Be stars, are known to vary in a complex way with no variability mechanism clearly identified. Aims. We attempt to characterize the optical variability of HD 37806 (MWC 120) on time scales ranging between minutes and several years. Methods. A continuous, one-minute resolution, 21 day-long sequence of MOST (Microvariability & Oscillations of STars) satellite observations has been analyzed using wavelet, scalegram and dispersion analysis tools. The MOST data have been augmented by sparse observations over 9 seasons from ASAS (All Sky Automated Survey), by previously non-analyzed ESO (European Southern Observatory) data partly covering 3 seasons and by archival measurements dating back half a century ago. Results. Mutually superimposed flares or accretion instabilities grow in size from about 0.0003 of the mean flux on a time scale of minutes to a peak-to-peak range of <0.05 on a time scale of a few years. The resulting variability has properties of stochastic "red" noise, whose self-similar characteristics are very similar to those observed in cataclysmic binary stars, but with much longer characteristic time scales of hours to days (rather than minutes) and with amplitudes which appear to cease growing in size on time scales of tens of years. In addition to chaotic brightness variations combined with stochastic noise, the MOST data show a weakly defined cyclic signal with a period of about 1.5 days, which may correspond to the rotation of the star.

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“…The stellar populations in the Ori OB1b association have been characterised after Blaauw's (1964) seminal work by many authors (Hardie et al 1964;Warren & Hesser 1978;Guetter 1981;Brown et al 1994;Hernández et al 2005). In contrast to the hypothesis of Sharpless (1962), who claimed a lack of noticeable excess of members in Ori OB1b later than A5, at least two nearby clusters are known within the association: σ Orionis, centred on the eponym σ Ori Trapezium-like star system (see above), and Collinder 70, centred on Alnilam (Collinder 1931).…”

Section: Alnilam and Mintakamentioning

confidence: 99%

Young stars and brown dwarfs surrounding Alnilam (ϵ Orionis) and Mintaka (δ Orionis)

Caballero

Solano

2008

A&A

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Aims. We look for new regions to search for substellar objects. Methods. Two circular areas, 45 arcmin-radius each, centred on the young massive star systems Alnilam and Mintaka in the Orion Belt, were explored. The regions are very young (less than 10 Ma), have low extinction, and are neighbours to σ Orionis (∼3 Ma), a young open cluster very rich in brown dwarfs and planetary-mass objects. We used Virtual Observatory tools, the astro-photometric Tycho-2, DENIS and 2MASS catalogues, 10 control fields at similar galactic latitudes, as well as X-ray, mid-infrared, and spectroscopic data from the literature. Results. We compiled exhaustive lists of known young stars and new candidate members in the Ori OB1b association and of foreand background sources. A total of 136 stars display features of extreme youth, like early spectral types, lithium in absorption, or mid-infrared flux excess. Other two young brown dwarf and 289 star candidates have been identified from an optical/near-infrared colour-magnitude diagram. We list another 74 known objects that might belong to the association. This catalogue can serve as input for characterising the stellar and high-mass substellar populations in the Orion Belt. Finally, we investigated the surface densities and radial distributions of young objects surrounding Alnilam and Mintaka and compared them with those in the σ Orionis cluster. We report on a new open cluster centred on Mintaka. Conclusions. Both regions can be analogues to the σ Orionis cluster, but more massive, more extended, slightly older, and less radially concentrated.

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A Study of the B Stars in the Orion Belt Region.

Cited by 14 publications

References 0 publications

Archaeoastronomical Study of the Main Pyramids of Giza, Egypt: Possible Correlations with the Stars?

Archaeoastronomical Study of the Main Pyramids of Giza, Egypt: Possible Correlations with the Stars?

Photometric variability of the Herbig Ae star HD 37806

Young stars and brown dwarfs surrounding Alnilam (ϵ Orionis) and Mintaka (δ Orionis)

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