The Complete Life-Cycle of a Butterfly

•Descargar como PPT, PDF•

1 recomendación•230 vistas

A female butterfly lays an egg on a leaf, which hatches into a caterpillar. The caterpillar eats constantly until wrapping itself in a cocoon for two weeks, emerging as a beautiful butterfly. Additional facts note that butterflies can see certain colors, have four wings and antennae to help see, with females generally larger than males as butterflies feed on nectar from flower to flower.

Ciencias Deportes Entretenimiento y humor

1. The Egg
• The female butterfly
lays an egg on a leaf.

2. Caterpillar
• Out of the egg
hatches a tiny
caterpillar.
• The caterpillar eats
and eats and eats.

3. The Chrysalis
• The caterpillar wraps
himself inside a
cocoon and stays
inside for about 2
weeks.

4. The Butterfly
• Out of the chrysalis
comes a beautiful
butterfly!

Butterfly Facts
• Butterflies can see red, green, and yellow.
• Butterflies have four wings.
• They have antennae that help them see.
• Female butterflies are bigger than male
butterflies.
• A butterfly flies from flower to flower eating
nectar.

Más contenido relacionado

Destacado

Here comes The Avengers!

VAST ONLINE TRAFFIC™

Earthquakes and Volcanoes

VAST ONLINE TRAFFIC™

The Avengers (short comic)

VAST ONLINE TRAFFIC™

The Definition of CLASSIFICATION

VAST ONLINE TRAFFIC™

PLNOG15: What about latency? - Piotr Jabłoński

PROIDEA

Nowadays, everyone knows about the great importance of SAP systems and the critical data processed by them. Large companies install SAP Security Notes regularly so as not to repeat the mistake of Nvidia. One bug is not enough anymore to get access to all corporate SAP systems. Pentesters frequently find themselves in a situation where the OS of an SAP server has been compromised successfully, but they have not got an access to the ERP system. In addition, it is rather common to have an unprivileged account, which give them access to the encrypted password, but not to the whole system. Sometimes they even try to break into other systems with help of the passwords, which users usually use in the systems they’ve already broken, but they can’t, because they need them to be decrypted first. Where do we find the treasured password to access the financial transactions and revenues of NASDAQ monsters? Where and how does SAP store user passwords? Are all passwords stored as hashes, or can attackers find passwords in plaintext? This talk reviews the many places where SAP stores critical credentials, such as usernames and passwords, and, which is more interesting, the way it stores them. Methods of retrieving them will be described, and decryption utilities will be presented. SAP GUI shortcuts, RFC connections, SAP Security Storage, logs, traces, Database links, SAP HANA Storage, you name it – all varieties of SAP modules will be discussed in this talk.

CONFidence 2014: Dimitriy Chastuhin: All your sap p@$$w0яd z belong to us

PROIDEA

JDD2014: Code review - jak zyskać więcej niż tracić? - Sebastian Malaca

PROIDEA

Motivation

Gc university faisalabad

The targetd of this presentation is to be for both sexes, all ages, all colors, creeds and faiths. It matters not if you’re a adolescent that has got ‘carried away’, a middle aged woman who’s simply spent her life savings or a individual sitting in his prison cell doing a long stretch for a problem gambling related condemnable offence. I’m not worried with whether the debt you discover yourself in is 1000, or one 1000000000000, our journey is more or less the same - you have to change. In my eyes the past may stop here and the future may begin here. For proven, professional help, visit these guys.. >> http://tinyurl.com/stoptogamble

GET RID OF GAMBLING ADDICTION - Overcome One Of The Most Difficult Addictions...

VAST ONLINE TRAFFIC™

Destacado (9)

Here comes The Avengers!

Earthquakes and Volcanoes

The Avengers (short comic)

The Definition of CLASSIFICATION

PLNOG15: What about latency? - Piotr Jabłoński

CONFidence 2014: Dimitriy Chastuhin: All your sap p@$$w0яd z belong to us

JDD2014: Code review - jak zyskać więcej niż tracić? - Sebastian Malaca

Motivation

GET RID OF GAMBLING ADDICTION - Overcome One Of The Most Difficult Addictions...

Último

family therapy psychotherapy types .pdf

haseebahmeddrama

Studying the escaping atmospheres of highly irradiated exoplanets is critical for understanding the physical mechanisms that shape the demographics of close-in planets. A number of planetary outflows have been observed as excess H/He absorption during/after transit. Such an outflow has been observed for WASP-69b by multiple groups that disagree on the geometry and velocity structure of the outflow. Here, we report the detection of this planet’s outflow using Keck/NIRSPEC for the first time. We observed the outflow 1.28 hr after egress until the target set, demonstrating the outflow extends at least 5.8 × 105 km or 7.5 Rp This detection is significantly longer than previous observations, which report an outflow extending ∼2.2 planet radii just 1 yr prior. The outflow is blueshifted by −23 km s−1 in the planetary rest frame. We estimate a current mass-loss rate of 1 M⊕ Gyr−1 . Our observations are most consistent with an outflow that is strongly sculpted by ram pressure from the stellar wind. However, potential variability in the outflow could be due to time-varying interactions with the stellar wind or differences in instrumental precision.

WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp

Sérgio Sacani

Cyanobacteria (also known as blue-green algae) are ubiquitous photosynthetic microorganisms found in diverse habitats such as fresh water, marine water, moist rocks, etc. The photosynthetic mode of nutrition makes them significant global oxygen producers along with nitrogen-fixing ability of heterocyst and carbon sequestration. Some cyanobacterial species have the ability to perform a dual mode of nutritional procurement. This unique capability of cyanobacteria to utilize both organic (heterotrophic) and inorganic (autotrophic) carbon sources for energy production and growth is termed as mixotrophy which impart nutritional flexibility and competitive ability to them. Cyanobacterial mixotrophy provides the promising avenues in biotechnological applications such as wastewater treatment, bioremediation, pharmaceuticals, food supplements, biofertilizer, coloring agents, synthesis of bioactive compounds and as an agent for eco-friendly bio-fuels generation, etc Mixotrophically grown cyanobacteria, demonstrate significant potential for efficient and economical applications beyond their conventional agricultural application, thereby offering a versatile and impactful resource for future technological and environmental challenges.

mixotrophy in cyanobacteria: a dual nutritional strategy

MansiBishnoi1

GBSN - Microbiology (Unit 6) Human and Microbial interaction

Areesha Ahmad

Lec 1.b Totipotency and birth of tissue culture.ppt

asifali1111

MODERN PHYSICS_REPORTING_QUANTA_.....pdf

RevenJadePalma

The highest priority recommendation of the Astro2020 Decadal Survey for space-based astronomy was the construction of an observatory capable of characterizing habitable worlds. In this paper series we explore the detectability of and interference from exomoons and exorings serendipitously observed with the proposed Habitable Worlds Observatory (HWO) as it seeks to characterize exoplanets, starting in this manuscript with Earth-Moon analog mutual events. Unlike transits, which only occur in systems viewed near edge-on, shadow (i.e., solar eclipse) and lunar eclipse mutual events occur in almost every star-planet-moon system. The cadence of these events can vary widely from ∼yearly to multiple events per day, as was the case in our younger Earth-Moon system. Leveraging previous space-based (EPOXI) lightcurves of a Moon transit and performance predictions from the LUVOIR-B concept, we derive the detectability of Moon analogs with HWO. We determine that Earth-Moon analogs are detectable with observation of ∼2-20 mutual events for systems within 10 pc, and larger moons should remain detectable out to 20 pc. We explore the extent to which exomoon mutual events can mimic planet features and weather. We find that HWO wavelength coverage in the near-IR, specifically in the 1.4 µm water band where large moons can outshine their host planet, will aid in differentiating exomoon signals from exoplanet variability. Finally, we predict that exomoons formed through collision processes akin to our Moon are more likely to be detected in younger systems, where shorter orbital periods and favorable geometry enhance the probability and frequency of mutual events.

Exomoons & Exorings with the Habitable Worlds Observatory I: On the Detection...

Sérgio Sacani

In this work, we assess the potential detectability of solar panels made of silicon on an Earth-like exoplanet as a potential technosignature. Silicon-based photovoltaic cells have high reflectance in the UV-VIS and in the near-IR, within the wavelength range of a space-based flagship mission concept like the Habitable Worlds Observatory (HWO). Assuming that only solar energy is used to provide the 2022 human energy needs with a land cover of ∼ 2.4%, and projecting the future energy demand assuming various growth-rate scenarios, we assess the detectability with an 8 m HWO-like telescope. Assuming the most favorable viewing orientation, and focusing on the strong absorption edge in the ultraviolet-to-visible (0.34 − 0.52 µm), we find that several 100s of hours of observation time is needed to reach a SNR of 5 for an Earth-like planet around a Sun-like star at 10pc, even with a solar panel coverage of ∼ 23% land coverage of a future Earth. We discuss the necessity of concepts like Kardeshev Type I/II civilizations and Dyson spheres, which would aim to harness vast amounts of energy. Even with much larger populations than today, the total energy use of human civilization would be orders of magnitude below the threshold for causing direct thermal heating or reaching the scale of a Kardashev Type I civilization. Any extraterrrestrial civilization that likewise achieves sustainable population levels may also find a limit on its need to expand, which suggests that a galaxy-spanning civilization as imagined in the Fermi paradox may not exist.

Detectability of Solar Panels as a Technosignature

Sérgio Sacani

SCHISTOSOMA HEAMATOBIUM life cycle .pdf

DebdattaGhosh6

Within the uncertainties of involved astronomical and biological parameters, the Drake Equation typically predicts that there should be many exoplanets in our galaxy hosting active, communicative civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing the importance of planetary tectonic style for biological evolution. We summarize growing evidence that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated emergence and evolution of complex species. We further suggest that both continents and oceans are required for ACCs because early evolution of simple life must happen in water but late evolution of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox (1) by adding two additional terms to the Drake Equation: foc (the fraction of habitable exoplanets with significant continents and oceans) and fpt (the fraction of habitable exoplanets with significant continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by demonstrating that the product of foc and fpt is very small (< 0.00003–0.002). We propose that the lack of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on exoplanets with primitive life.

The importance of continents, oceans and plate tectonics for the evolution of...

Sérgio Sacani

Mammals have dominated Earth for approximately 55 Myr thanks to their adaptations and resilience to warming and cooling during the Cenozoic. All life will eventually perish in a runaway greenhouse once absorbed solar radiation exceeds the emission of thermal radiation in several billions of years. However, conditions rendering the Earth naturally inhospitable to mammals may develop sooner because of long-term processes linked to plate tectonics (short-term perturbations are not considered here). In ~250 Myr, all continents will converge to form Earth’s next supercontinent, Pangea Ultima. A natural consequence of the creation and decay of Pangea Ultima will be extremes in pCO2 due to changes in volcanic rifting and outgassing. Here we show that increased pCO2, solar energy (F⨀; approximately +2.5% W m−2 greater than today) and continentality (larger range in temperatures away from the ocean) lead to increasing warming hostile to mammalian life. We assess their impact on mammalian physiological limits (dry bulb, wet bulb and Humidex heat stress indicators) as well as a planetary habitability index. Given mammals’ continued survival, predicted background pCO2 levels of 410–816 ppm combined with increased F⨀ will probably lead to a climate tipping point and their mass extinction. The results also highlight how global landmass configuration, pCO2 and F⨀ play a critical role in planetary habitability.

Climate extremes likely to drive land mammal extinction during next supercont...

Sérgio Sacani

Triploidy ...............................pptx

Cherry

Land use land cover change analysis and detection of its drivers using geospa...

MohammedAhmed246550

Plasmapheresis - Dr. E. Muralinath - Kalyan . C.pptx

muralinath2

Mining Activity and Investment Opportunity in Myanmar.pptx

KyawThanTint

Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days. The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of 3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric (TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.

Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...

Sérgio Sacani

PESTS OF GREEN MANURE CROPS AND FORAGE CROPS SESBANIA BORERS 1. Sesbania stem borer, Azygophleps scalaris, Cossidae, Lepidoptera Symptom of damage: Drying of sesbania plants. Nature of damage: Stoutly built larva bores into the stem and feeds, the faecal matter getting accumulated at the entrance hole. Egg: Laid in masses attached to the leaflets. Larva: Robust larva of 7 cm length, light brown with a reddish brown head. Pupa: Pupa has spines anteriorly with the help of which it moves up and down inside the tunnel in the stem. Adult: Sluggish yellowish brown moth. 2. Stem weevil, Alcidodes bubo, Curculionidae, Coleoptera Symptom of damage: Drying of the terminal branches or whole plant, lodging of the plants during monsoon seasons; affected stem with numerous bore holes and swelling symptoms. Presence of apodous grub inside the stem. Nature of damage: Grubs riddle into stem and cause thickenings on stem. The growth and vigour of the plants are impaired to a great extent. Egg: Laid on the stem. Grub : Apodous whitish grub. Adult: Reddish brown weevil with white transverse markings on the elytra. LEAF FEEDERS 3. Green semilooper, Pericyma glaucinans, Noctuidae, Lepidoptera Symptom of damage: Defoliation of plants preceding with leaflets damage. Nature of damage: Caterpillar feeds on the leaflets remaining along the ribs of leaves. Larva : Pale green, semilooper with broad yellow lateral stripes. Adult: Dark brown with black lines 4. Green looper, Semiothisa pervelgata, Semiothisa emersaria, Geometridae, Lepidoptera Symptom of damage: Defoliation of plants preceding with leaflets damage. Nature of damage: Larvae feed on the leaves. Egg: Oval greenish eggs laid singly on leaves. Larva : Pale green looper with white lines and when full grown becomes pink with horizontal bands of violet patches dorsally on the abdominal segments. Pupa: Pupates in the soil. Adult: White colour with three dark lines and spots on the wings.

Pests of Green Manures_Bionomics_IPM_Dr.UPR.pdf

PirithiRaju

ERTHROPOIESIS: Dr. E. Muralinath & R. Gnana Lahari

muralinath2

In the Nice model of solar system formation, Uranus and Neptune undergo an orbital upheaval, sweeping through a planetesimal disk. The region of the disk from which material is accreted by the ice giants during this phase of their evolution has not previously been identified. We perform direct N-body orbital simulations of the four giant planets to determine the amount and origin of solid accretion during this orbital upheaval. We find that the ice giants undergo an extreme bombardment event, with collision rates as much as ∼3 per hour assuming km-sized planetesimals, increasing the total planet mass by up to ∼0.35%. In all cases, the initially outermost ice giant experiences the largest total enhancement. We determine that for some plausible planetesimal properties, the resulting atmospheric enrichment could potentially produce sufficient latent heat to alter the planetary cooling timescale according to existing models. Our findings suggest that substantial accretion during this phase of planetary evolution may have been sufficient to impact the atmospheric composition and thermal evolution of the ice giants, motivating future work on the fate of deposited solid material.

Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Mat...

Sérgio Sacani

Plasma proteins_ Dr.Muralinath_Dr.c. kalyan

muralinath2