Abundance Analysis of a Sample of Bipolar Type I Planetary Nebulae

2005 ◽  
Author(s):  
O. Lorente-Espin
Keyword(s):  
Planetary Nebulae ◽  
Type I ◽  
Bipolar Type

Bipolar Type I Disorder in Children

2020 ◽  
Vol 1 (1) ◽  
pp. 11-14
Author(s):  
Syaiful Fadilah ◽  
Fatimah Haniman
Keyword(s):  
Bipolar Disorder ◽  
Children And Adolescents ◽  
Severe Disease ◽  
Large Population ◽  
Type I ◽  
Disease Course ◽  
Clinical Area ◽  
Clinical Disorder ◽  
Bipolar Type ◽  
Dsm Iv

Bipolar disorder in children and adolescents is a clinical disorder that causes publicmental health problems that need attention. In the last decade, bipolar disorder in children andadolescents has become a trendy field, both in the clinical area and in research, especially interms of diagnosis, which is still controversial. The controversy that remains is whether it ispossible to diagnose bipolar disorder in prepubertal children. Based on the DSM-IV-TRdiagnostic criteria, the prevalence of the bipolar disorder in children scarce rare.Epidemiological studies report the lifetime prevalence of bipolar I and II disorders in lateadolescence is about 1 per cent. Various studies in a large population have shown aprevalence rate of 0.1% -2%. The onset of bipolar disorder in children and adolescents is oftenaccompanied by a more severe disease course, compared to bipolar disorder with onset inadulthood. This case report presents a case of bipolar 1 in children accompanied bycomprehensive management.

Planetary Nebulae of Type I Revisited

1997 ◽  
pp. 175-183 ◽  
Author(s):  
S. Torres-Peimbert ◽  
M. Peimbert
Keyword(s):  
Planetary Nebulae ◽  
Type I

Spectrophotometry of Selected Planetary Nebulae of Type I in the Magellanic Clouds

1993 ◽  
pp. 584-584
Author(s):  
S. Torres-Peimbert ◽  
M. Peimbert ◽  
M. T. Ruitz ◽  
M. Peña
Keyword(s):  
Planetary Nebulae ◽  
Magellanic Clouds ◽  
Type I

scholarly journals Helium and Oxygen Abundances in SMC Planetary Nebulae

2000 ◽  
Vol 198 ◽  
pp. 234-235
Author(s):  
R. D. D. Costa ◽  
J. A. de Freitas Pacheco ◽  
T. P. Idiart
Keyword(s):  
Spectroscopic Data ◽  
Planetary Nebulae ◽  
Hii Regions ◽  
Physical Parameters ◽  
Type I ◽  
Chemical Abundances ◽  
High Quality

In this work we report new high quality spectroscopic data for a sample of PNe in the SMC, aiming to derive physical parameters and chemical abundances, in particular to settle the question concerning the oxygen discrepancy found for type I planetaries with respect to stars and HII regions.

scholarly journals N/O Abundances in Planetary Nebulae from Far-Infrared Line Observations

1989 ◽  
Vol 131 ◽  
pp. 214-214
Author(s):  
Harriet L. Dinerstein ◽  
Michael W. Werner
Keyword(s):  
Planetary Nebulae ◽  
Far Infrared ◽  
Optical Observations ◽  
Type I ◽  
Local Electron ◽  
Extreme Type ◽  
Order Of Magnitude ◽  
Progenitor Stars ◽  
Infrared Array ◽  
Atomic Parameters

Measurements of the [O III] 52, 88 μm and [N III] 57 μm fine-structure emission lines have been obtained for nine planetary nebulae, using the facility far-infrared array spectrometer on NASA's Kuiper Airborne Observatory. The N++/O++ ratios determined from these observations range by more than an order of magnitude among the sample. Using recent improved values for the atomic parameters, we find that the N++/O++ ratios agree fairly well with values of N+/O+ determined from optical lines in the same objects. The highest N++/O++ values, found for the extreme “Type I” nebulae NGC 2440 and NGC 6302, are approximately unity. These results imply that the synthesis and mixing of nitrogen must be extremely efficient in the progenitor stars of some planetary nebulae, and that these nebulae are significant sources of nitrogen to the interstellar medium. The local electron densities derived from the intensity ratios of the two [O III] lines are generally lower than values in the literature determined from small-beam optical observations of other ions, such as [O II]. This effect can be understood in terms of the presence of clumpy structure in the nebula, since the far-infrared lines have fairly low critical densities for collisional de-excitation and therefore are preferentially emitted from low-density gas.

scholarly journals Hubble Space Telescope Images of Four Magellanic Cloud Planetary Nebulae

1993 ◽  
Vol 155 ◽  
pp. 213-213
Author(s):  
M. J. Barlow ◽  
J. C. Blades ◽  
S. Osmer ◽  
Keyword(s):  
Hubble Space Telescope ◽  
Planetary Nebulae ◽  
Circular Ring ◽  
Uniform Structure ◽  
Full Description ◽  
Type I ◽  
Space Telescope ◽  
Ring Shape ◽  
Faint Object ◽  
Northern Edge

Using the Faint Object Camera on-board the Hubble Space Telescope, we have obtained images of four planetary nebulae in the Magellanic Clouds, namely N2 and N5 in the SMC and N66 and N201 in the LMC. Each nebula was imaged through narrow-band filters isolating [O III] λ5007 and Hβ, for a nominal exposure time of 1000 seconds in each filter. The f/96 optical chain of the FOC was used, yielding 512×512 0.022 arcsec square pixels. Considerable detail is evident on the raw images and after deconvolution using the Richardson-Lucy algorithm, structures as small as 0.06 arcsec are easily discernible. Figure 1 shows NS and EW intensity cross-cuts through the deconvolved [O III] λ5007 images of SMC N2 and SMC N5. SMC N2 is a slightly ellleptical ringlike nebula, with its greatest elongation in the EW direction. The peak-to-peak dimensions of the ring are 0.21×0.26 arcsec2. SMC N5 has a circular ring shape, with the [O III] λ5007 image showing a clearly defined, nearly uniform structure, apart from a bright patch at the northern edge. The peak-to-peak diameter of the ring is 0.26 arcsec and the ring itself is significantly narrower than that of SMC N2, with a width as small as 0.06 arcsec (FWHM) in some places. LMC N201 is very compact, with a FWHM of 0.21 arcsec in the Hβ image. The Type I PN LMC N66 is a multi-polar nebula, with the brightest part having an extent of about 2 arcsec. Its structure is extremely complex, with several bright knots and faint loops visible outside the two bright lobes. A full description of our results can be found in Blades et al., ApJ,398, L41–44.

Planetary Nebulae in the SMC

2003 ◽  
Vol 209 ◽  
pp. 625-628 ◽  
Author(s):  
George H. Jacoby ◽  
Orsola De Marco ◽  
Robin Ciardullo
Keyword(s):  
Planetary Nebula ◽  
Luminosity Function ◽  
Planetary Nebulae ◽  
Type I ◽  
Complete Survey ◽  
New Feature

Using the ESO 2.2m telescope with the 8K x 8K mosaic CCD, we surveyed 2.8 square degrees (~1.6° x 1.7°) of the SMC to search for faint planetary nebulae (PN). In this region, 34 PN were previously known; we identified 25 new objects. All of these are faint and have been spectroscopically confirmed. We estimate that there should be ~140 PN in the entire SMC to the limits of a survey like this one, which is complete to 6 mag down the planetary nebula luminosity function (PNLF). For a complete survey (8 mag down the PNLF), there should be ~220 PN. A strong new feature is evident in the PNLF as a deficiency at 4 mags below the brightest PN.The survey spectra that were used to confirm the candidates as PN show that the fainter PN exhibit a higher incidence (~28%) of strong [N II] emission (where I([N II]/I(Hα) > 1) relative to the bright Sanduleak et al. (1978) sample (~6%). We propose that the very faint SMC PN are selectively biased toward the chemically enriched Type I objects derived from younger, more massive progenitors.

The role of shocks in the determination of empirical abundances for type-I PNe

2018 ◽  
Vol 14 (S343) ◽  
pp. 377-378
Author(s):  
Roberto D. D. Costa ◽  
Paulo J. A. Lago
Keyword(s):  
Planetary Nebulae ◽  
Type I ◽  
Correction Factors ◽  
Chemical Abundances

AbstractWe investigate, in the light of new diagnostic diagrams, the role of shocks in the ionization profile of type-I planetary nebulae, and their relation to the empirical derivation of chemical abundances. We apply our technique to two well-known type-I objects: NGC 2440 and NGC 6302. Our results indicate that shocks play a very important role in the spectra of both nebulae and, since the presence of shocks reinforces the flux of low ionization lines, this artificial reinforcement can lead to incorrect chemical abundances, when they are derived through Ionization Correction Factors, at least for type-I PNe.

Psychosocial Treatment for Bipolar Disorder

CNS Spectrums ◽  
2010 ◽  
Vol 15 (S3) ◽  
pp. 14-16
Author(s):  
Noreen Reilly-Harrington
Keyword(s):  
Bipolar Disorder ◽  
Collaborative Care ◽  
Medication Compliance ◽  
Behavioral Therapy ◽  
Mood Stabilizer ◽  
Psychosocial Treatment ◽  
Psychoeducational Intervention ◽  
Type I ◽  
Bipolar Type ◽  
Social Rhythm

Medication is the mainstay of treatment for bipolar disorder. However, no medication will be effective if patients do not take it, and the rates of medication compliance in bipolar disorder are very low. Johnson and McFarland found that the modal length of compliance with a mood stabilizer was only 2 months. Keck and colleagues found that 50% to 66% of patients with bipolar disorder exhibit poor compliance within the first 12 months of treatment. In addition, even with adequate medication compliance, high rates of relapse persist.Adjunctive psychosocial treatments can help reduce relapse and provide patients as well as their families with tools to manage bipolar disorder more effectively. Several forms of intensive psychotherapy have shown promise for the treatment of bipolar disorder. In the Systematic Treatment Enhancement Program for Bipolar Disorder, Miklowitz and colleagues compared three forms of intensive interventions: cognitive-behavioral therapy (CBT), interpersonal and social rhythm therapy, and family-focused treatment. These were compared to a brief, 3-session psychoeducational intervention known as collaborative care. A total of 293 depressed patients with bipolar type I or type II disorder were treated with protocol pharmacotherapy and were randomly assigned to either one of the three intensive interventions or the brief psychoeducational intervention.The three intensive interventions provided up to 30 sessions of treatment over a 9-month period. The collaborative care intervention consisted of three sessions administered over a 6-week period. The authors found that patients who received one of the intensive interventions had a median time to recovery 110 days earlier than patients who had received the collaborative care conditions. Patients who received one of the three intensive psychotherapies also had significantly higher year-end recovery rates, and are more than 1 to 1.5 times more likely to be clinically well during any study month. No statistically significant differences were found between the 3 intensive treatments.

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