<i>A priori</i> design of a photoreactor for the chlorination of ethane

Clariá, M. A.; Irazoqui, Horacio Antonio; Cassano, Alberto E.

doi:10.1002/aic.690340303

Cited by 36 publications

(51 citation statements)

References 44 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…Unless the agreement between the spatial and velocity information of these two regions is a coincidence, we can use the distance of the H II region as an estimate of the distance to the filament. The distance to the CMa OB1 association has been determined photometrically by Clariá (1974) to be 1150 ± 140 pc, consistent with a kinematic distance of 800-1100 pc for the Hα emitting gas in the region (Reynolds & Ogden 1978). In this letter, we adopt a distance of 1 kpc for Filament 1 but include d 1 = d/1 kpc in the derived parameters.…”

Section: Discussionsupporting

confidence: 68%

Faint, Large-Scale Hα Filaments in the Milky Way

Haffner

Reynolds

Tufte

1998

The Astrophysical Journal

View full text Add to dashboard Cite

During the initial data reduction of the Wisconsin H-Alpha Mapper (WHAM) Hα Sky Survey, we have discovered several very long (∼ 30 • -80 • ) filaments superimposed on the diffuse Hα background. These features have no clear correspondence to the other phases of the interstellar medium revealed by 21 cm, X-ray, IR, or radio continuum surveys, and they have no readily identifiable origin or source of ionization. In this letter, the data for two of these faint (I Hα ≈ 0.5-1.5 R) structures are presented. The first is an 80 • -long, 2 • -wide arch that extends nearly perpendicular to the Galactic plane at ℓ = 225 • and attains a maximum latitude of +51 • near ℓ = 240 • before reaching the southern boundary of our survey map at ℓ = 270 • , b = +42 • . The vertical portion of this feature between b = +10 • and +25 • is associated with a single radial velocity component centered at v LSR = +16 km s −1 with a full width at half maximum of 27 km s −1 . A decrease in the velocity is observed from b = +33 • through +48 • as the feature arches toward higher Galactic longitudes. At this end, the emission component is centered near v LSR = −20 km s −1 . Where this feature appears to meet the Galactic plane near ℓ = 225 • , it is directly above the H II region surrounding CMa R1/OB1. A second filament consists of a ∼ 25 • -30 • -long arc spanning ℓ = 210 • -240 • at b = +30 • to 40 • . The radial velocity of this feature increases systematically from 0 km s −1 at ℓ = 215 • , b = +38 • to +18 km s −1 at ℓ = 236 • , b = +28 • . Both features have rather constant intensities along their entire lengths, ranging from 0.5-1.5 R (EM = 1-3 cm −6 pc) with no obvious trends.

show abstract

Section: Discussionsupporting

confidence: 68%

Faint, Large-Scale Hα Filaments in the Milky Way

Haffner

Reynolds

Tufte

1998

The Astrophysical Journal

View full text Add to dashboard Cite

show abstract

“…In the second case the discretization is automatic. According to Clariá et al (1988) we can treat the problem as follows. Consider for example the case of the LVRPA:…”

Section: The Radiation Balancementioning

confidence: 99%

Photocatalytic intrinsic reaction kinetics I: Mineralization of dichloroacetic acid

Zalazar

Romero

Martín

et al. 2005

Chemical Engineering Science

View full text Add to dashboard Cite

“…The value of the LVRPA is defined for monochromatic radiation but it can be extended to polychromatic fields by performing an integration over all useful wavelengths. The useful wavelength range is defined by the overlapping ranges of lamp emission, region of reactor wall good transmission properties, reactant or catalyst absorption, and, eventually, reflector reflectance (Clariá et al, 1988).…”

Section: Radiation Transportmentioning

confidence: 99%

Design and Analysis of Homogeneous and Heterogeneous Photoreactors

Cassano

Alfano

2005

Chemical Engineering

View full text Add to dashboard Cite

It is an impossible task for a short chapter to carryout a complete discussion of photoreactoreactor analysis and design unless we assume that the readers of this work have a previous background in the subject and chemical engineering fundamentals. Moreover, we can increase the chapter's feasibility if coverage is restricted to only a fraction, albeit a significant fraction, of the homogeneous and heterogeneous photoreactions. On this basis, it is possible to concentrate on those aspects that are distinctive of homogeneous photochemical and heterogeneous photocatalytic processes. For more details, the reader is referred to the original publications listed in the references.The distinctive aspect of these reactions is the unavoidable existence of a radiation field inside the reactor, which only in very special and unusual cases can be considered uniform in space and frequently is not even constant in time. This is because inside the reaction space, besides geometrical effects produced by the characteristics of the reactor geometry, there must be absorption of radiation to produce the reaction activation. This absorption means attenuation of the incoming intensities; i.e. without attenuation, there is no photochemical reaction. In some heterogeneous systems, scattering is another source of variation in the incoming rays. Hence, spatial variations are unavoidable. These intrinsic non-uniformities, unfortunately often neglected or not properly accounted for, are responsible for the majority of the difficulties associated with photoreactor analysis and design.Many different shapes and configurations are possible for either single-phase or multiphase reactors (Braun et al

show abstract

A priori design of a photoreactor for the chlorination of ethane

Cited by 36 publications

References 44 publications

Faint, Large-Scale Hα Filaments in the Milky Way

Faint, Large-Scale Hα Filaments in the Milky Way

Photocatalytic intrinsic reaction kinetics I: Mineralization of dichloroacetic acid

Design and Analysis of Homogeneous and Heterogeneous Photoreactors

Contact Info

Product

Resources

About