Personality Change and Prognosis After Leucotomy

Garmany, Gerald

doi:10.1192/bjp.94.395.428

Cited by 20 publications

(18 citation statements)

References 9 publications

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“…Only 1 of the 4 (HD209961, HIP109082, B2V) spectroscopic binaries discussed by van Albada & Klomp (1969) is selected. Several other studies have put forward 'special' candidate members (e.g., Crawford 1961;Slettebak, Bahner & Stock 1961;Kodaira, Greenstein & Oke 1970;Levato & Abt 1976;Guetter 1976;Malaroda 1981;Garmany & Stencel 1992): we confirm membership of the emission-line star HD216851 (HIP113226, B3V:n), the shell star HD213801 (HIP111337, B9V), and the red supergiants HD213310 and HD216946 (HIP111022, M0II, and HIP113288, K5Ibvar, respectively). We do not confirm most candidate members with peculiar and/or magnetic spectra.…”

Section: Lacerta Ob1supporting

confidence: 61%

“…The large variety in stellar content, projected dimension, clumpiness, age, and connection to the interstellar medium introduces biases in the identification of the associations. For example, associations containing several luminous supergiants can be detected out to several kpc (e.g., Cep OB1 in §8.2 ;Humphreys 1978;Garmany & Stencel 1992), whereas associations without such stars can easily escape attention. Ruprecht's list is based on Ambartsumian's definition which requires the presence of O stars and an open cluster as 'nucleus' (e.g., Alter et al 1970).…”

Section: The Solar Neighbourhoodmentioning

confidence: 99%

“…The corresponding physical dimensions, 240 pc × 50 pc, make a common origin for these stars implausible (cf. Garmany & Stencel 1992). Humphreys (1978) compiled a list of 19 luminous stars for Cam OB1 based on positions, photometric distances and, when available, radial velocities.…”

Section: Cassiopeia-taurus and α Persei (Per Ob3)mentioning

confidence: 99%

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A [ITAL]Hipparcos[/ITAL] Census of the Nearby OB Associations

Zeeuw¹,

Hoogerwerf²,

Bruijne³

et al. 1999

The Astronomical Journal

1,205

118

1,616

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A comprehensive census of the stellar content of the OB associations within 1 kpc from the Sun is presented, based on Hipparcos positions, proper motions, and parallaxes. It is a key part of a long-term project to study the formation, structure, and evolution of nearby young stellar groups and related star-forming regions.OB associations are unbound 'moving groups', which can be detected kinematically because of their small internal velocity dispersion. The nearby associations have a large extent on the sky, which traditionally has limited astrometric membership determination to bright stars (V ∼ < 6 m ), with spectral types earlier than ∼B5. The Hipparcos measurements allow a major improvement in this situation. Moving groups are identified in the Hipparcos Catalogue by combining de Bruijne's refurbished convergent point method with the 'Spaghetti method' of Hoogerwerf & Aguilar. Astrometric members are listed for 12 young stellar groups, out to a distance of ∼650 pc. These are the 3 subgroups Upper Scorpius, Upper Centaurus Lupus and Lower Centaurus Crux of Sco OB2, as well as Vel OB2, Tr 10, Col 121, Per OB2, α Persei (Per OB3), Cas-Tau, Lac OB1, Cep OB2, and a new group in Cepheus, designated as Cep OB6. The selection procedure corrects the list of previously known astrometric and photometric B-and A-type members in these groups, and identifies many new members, including a significant number of F stars, as well as evolved stars, e.g., the Wolf-Rayet stars γ 2 Vel (WR11) in Vel OB2 and EZ CMa (WR6) in Col 121, and the classical Cepheid δ Cep in Cep OB6. Membership probabilities are given for all selected stars. Monte Carlo simulations are used to estimate the expected number of interloper field stars. In the nearest associations, notably in Sco OB2, the later-type members include T Tauri objects and other stars in the final pre-main sequence phase. This provides a firm link between the classical high-mass stellar content and ongoing low-mass star formation. Detailed studies of these 12 groups, and their relation to the surrounding interstellar medium, will be presented elsewhere.Astrometric evidence for moving groups in the fields of R CrA, CMa OB1, Mon OB1, Ori OB1, Cam OB1, Cep OB3, Cep OB4, Cyg OB4, Cyg OB7, and Sct OB2, is inconclusive. OB associations do exist in many of these regions, but they are either at distances beyond ∼500 pc where the Hipparcos parallaxes are of limited use, or they have unfavorable kinematics, so that the group proper motion does not distinguish it from the field stars in the Galactic disk.The mean distances of the well-established groups are systematically smaller than the pre-Hipparcos photometric estimates. While part of this may be caused by the improved membership lists, a recalibration of the upper main sequence in the Hertzsprung-Russell diagram may be called for. The mean motions display a systematic pattern, which is discussed in relation to the Gould Belt.Six of the 12 detected moving groups do not appear in the classical list of nearby OB associations. This is sometim...

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Section: Lacerta Ob1supporting

confidence: 61%

Section: The Solar Neighbourhoodmentioning

confidence: 99%

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A [ITAL]Hipparcos[/ITAL] Census of the Nearby OB Associations

Zeeuw¹,

Hoogerwerf²,

Bruijne³

et al. 1999

The Astronomical Journal

1,205

118

1,616

View full text Add to dashboard Cite

show abstract

“…They are also essential for stars with weak winds, when H α turns into an almost photospheric absorption line, a situation impossible to deal with quantitatively by treating photosphere and wind as separated entities. For our work, we use the new unified model Garmany & Stencel, 1992 code developed recently by Santolaya-Rey et al (1997, hereafter SPH). This new code is extremely fast and produces a unified model in few minutes on a work station, which is crucial for a project aiming at the analysis of many stars with different stellar parameters and different wind properties.…”

Section: Model Atmospheres For the Stellar Wind Analysismentioning

confidence: 99%

The Wind Momentum – Luminosity Relationship of Blue Supergiants

Kudritzki

1999

International Astronomical Union Colloquium

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Abstract. The prediction of the Wind Momentum -Luminosity Relationship (WLR) based on the theory of radiation driven winds is verified by quantitative spectroscopy of winds of A-, B-and O-supergiants. The relationship depends on spectral type. New stellar wind calculations are presented reproducing the observed spectral type dependence. The impact of spectral variability on the WLR is investigated by an analysis of some hundred spectra of the luminous AOIa-supergiant HD92207 obtained within the Heidelberg Spectral Variability Survey and found to be small.Finally, the WLR is discussed as a tool for the determination of extragalactic distances. Recent results obtained for the Galaxy, M31 and M33 are presented. The potential of the method is discussed with the conclusion that it may allow independent distance moduli to be obtained with an accuracy of ten percent out to the Virgo and Fornax clusters of galaxies.

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“…Clinical Features.-Most writers have not given any clinical detail of their relapsed leucotomy cases, but Cook (1946) has described two patients with agitated depression who relapsed after one and a half years, and two with " somatopsychic "delusions who relapsed after four to five months; Frank (1946) referred to two paraphrenics who relapsed after one year and one aggressive psychopath who relapsed eight months after operation; and Garmany (1948) has reported an acutely obsessional patient with full relapse after complete postoperative recovery over a period of four years, and a catatonic who relapsed after three years of mental health. The types of mental symptoms and syndromes in these patients who suffered relapse and in the six under review comprise, therefore, most of the commonest components of the functional psychoses.…”

Section: Discussionmentioning

confidence: 99%