Causes and damage to fruits and vegetables during shipment / by J.W. Lloyd and H.M. Newell.

Lloyd, John William; Newell, H. M.

doi:10.5962/bhl.title.16653

Cited by 2 publications

(4 citation statements)

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“…Most CNe and RNe emit hard X-rays in the first months of the outburst with L X peaking at ∼10 33 -10 34 erg s −1 and bremsstrahlung temperatures in the range 0.5-20 keV (e.g., Orio et al 2001a, and references therein). The eclipsing, fast (t 3 ≃3 days * ) CN V838 Her (Nova Her 1991) was detected in hard X-rays 5 days after the outburst, with a kT ∼10 keV bremsstrahlung spectrum (Lloyd et al 1992). The hard emission generally lasts for at least ≃2 years and even much longer under special circumstances like pre-existing circumstellar material, or a prolonged wind phase (e.g., Orio et al 2001a).…”

Section: Hard X-ray Emissionmentioning

confidence: 99%

“…Alternatively, shocks may occur in the ejected shells during the different phases of the nova outburst. The expected hard X-ray spectrum is thermal, with kT eff ∼0.2-15 keV, depending on how much time has elapsed since the shock, and how efficient the cooling is, and with L X ≃10 33 -10 34 erg s −1 (e.g., Lloyd et al 1992;O'Brien et al 1994). Additionally a collection of emission lines are expected.…”

Section: The CV Two-qpo Diagrammentioning

confidence: 99%

“…The eclipsing, fast (t 3 ≃3 days * ) CN V838 Her (Nova Her 1991) was detected in hard X-rays 5 days after the outburst, with a kT ∼10 keV bremsstrahlung spectrum (Lloyd et al 1992). The hard emission generally lasts for at least ≃2 years and even much longer under special circumstances like pre-existing circumstellar material, or a prolonged wind phase (e.g., Orio et al 2001a).…”

Section: Hard X-ray Emissionmentioning

confidence: 99%

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X-rays from cataclysmic variables

Kuulkers

Norton

Schwope

et al. 2006

Compact Stellar X-Ray Sources

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IntroductionCataclysmic Variables * (CVs) are a distinct class of interacting binaries, transferring mass from a donor star to a degenerate accretor, a white dwarf (WD). In all observational determinations, and as is required by theory for stable mass transfer, the donor star is of lower mass than the accretor.The majority of CVs have orbital periods, P orb , between 75 min and 8 h (see Ritter & Kolb 2003) and consist of Roche Lobe-filling main sequence donors and WDs. These are WD analogues of the low-mass X-ray binaries (LMXBs; see Chapter 1). In the period range 8 h-3 d the donors must have larger radii than dwarfs in order to fill their Roche Lobes and are therefore evolved subgiants. A few CVs are found with P orb ∼200 d, which require giant donors for them to be Lobe-filling. The absence of evolved CVs with periods ∼3 to ∼200 d is connected with the dynamical instability that results from an initial donor that had a mass larger than about 67% of that of the WD; such binaries will have experienced rapid mass transfer and shortened their periods during a common envelope phase. Beyond P orb ∼200 d, mass-transferring systems also exist. These constitute the symbiotic binaries (SBs) and are in general not Roche Lobe-filling, but instead consist of a WD orbiting in the wind of a supergiant, and are thus analogues of the high-mass X-ray binaries (see Chapter 1).At the short end of the period range a different kind of CV exists, i.e., in which the mass losing donors are themselves WDs; they are entirely deficient in hydrogen. These helium-transferring CVs are known, after the type star, as AM CVn stars and are observed to have P orb from 60 min down to at least as short as 10 min. They have evolved by passage through two common envelope phases, which leaves the cores of both of the component stars exposed.The CVs are divided into subtypes. These were originally based entirely on the behaviour seen in long-term optical light curves, but to this are now added more subtle parameters such as the presence of polarisation. In essence, a CV's gross behaviour is determined by the rate of mass transfer from the donor,Ṁ donor , and * See Hack & La Dous (1993) and Warner (1995) for comprehensive overviews.

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Section: Hard X-ray Emissionmentioning

confidence: 99%

Section: The CV Two-qpo Diagrammentioning

confidence: 99%

Section: Hard X-ray Emissionmentioning

confidence: 99%

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X-rays from cataclysmic variables

Kuulkers

Norton

Schwope

et al. 2006

Compact Stellar X-Ray Sources

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“…This has been accelerated by the wave of takeovers, which has created greater scope for rationalisation' [23]. A survey of eleven large pharmaceutical companies with sites in the UK, found that only one had not been subject to either merger, take-over or the divestment of large parts of the business [24].…”

Section: The Pharmaceutical Industrymentioning

confidence: 99%